# Sun

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Names True-color image taken in 2019 using a solar filter Sun, Sol , [1] Sól, Helios [2] Solar [3] 1  AU ≈ 1.496×108 km [4] 8 min 19 s at light speed −26.74 [5] 4.83 [5] G2V [6] Z = 0.0122 [7] 31.6–32.7 minutes of arc [8] 0.527–0.545 degrees ≈26,660  light-years (2.25–2.50)×108 yr ≈251 km/s (orbit around the center of the Milky Way) ≈ 20 km/s (relative to average velocity of other stars in stellar neighborhood) ≈ 370 km/s [9] (relative to the cosmic microwave background) 695,700  km, [10] 696,342 km [11] [12] 4.379×106 km [12] 109 × Earth [12] 9×10−6 6.09×1012 km2 [12] 12,000 × Earth [12] 1.41×1018 km3 [12] 1,300,000 × Earth 1.9885×1030 kg [5] 332,950  Earths [5] 1.408 g/cm3 [5] [12] [13] 0.255 × Earth [5] [12] 162.2 g/cm3 [5] 12.4 × Earth 274 m/s2 [5] 28 × Earth [12] 0.070 [5] (estimate) 617.7 km/s [12] 55 × Earth [12] Center (modeled): 1.57×107 K [5] Photosphere (effective): 5,772  K [5] Corona: ≈ 5×106 K 3.828×1026  W [5] ≈ 3.75×1028  lm ≈ 98 lm/W efficacy 0.63 2.009×107 W·m−2·sr−1 ≈4.6 billion years (4.6×109 years) [14] [15] 73.46% hydrogen [16] 24.85% helium 0.77% oxygen 0.29% carbon 0.16% iron 0.12% neon 0.09% nitrogen 0.07% silicon 0.05% magnesium 0.04% sulphur 7.25° [5] (to the ecliptic)67.23°(to the galactic plane) 286.13°19 h 4 min 30 s +63.87°63° 52' North 25.05 days at equator25.38 days at 16° latitude34.4 days at poles [5] 1.997 km/s [12]

The Sun is the star at the center of the Solar System. It is a nearly perfect ball of hot plasma, [18] [19] heated to incandescence by nuclear fusion reactions in its core. The Sun radiates this energy mainly as light, ultraviolet, and infrared radiation, and is the most important source of energy for life on Earth.

## Contents

The Sun's radius is about 695,000 kilometers (432,000 miles), or 109 times that of Earth. Its mass is about 330,000 times that of Earth, comprising about 99.86% of the total mass of the Solar System. [20] Roughly three-quarters of the Sun's mass consists of hydrogen (~73%); the rest is mostly helium (~25%), with much smaller quantities of heavier elements, including oxygen, carbon, neon, and iron. [21]

The Sun is a G-type main-sequence star (G2V). As such, it is informally, and not completely accurately, referred to as a yellow dwarf (its light is actually white). It formed approximately 4.6 billion [lower-alpha 1] [14] [22] years ago from the gravitational collapse of matter within a region of a large molecular cloud. Most of this matter gathered in the center, whereas the rest flattened into an orbiting disk that became the Solar System. The central mass became so hot and dense that it eventually initiated nuclear fusion in its core. It is thought that almost all stars form by this process.

Every second, the Sun's core fuses about 600 million tons of hydrogen into helium, and in the process converts 4 million tons of matter into energy. This energy, which can take between 10,000 and 170,000 years to escape the core, is the source of the Sun's light and heat. When hydrogen fusion in its core has diminished to the point at which the Sun is no longer in hydrostatic equilibrium, its core will undergo a marked increase in density and temperature while its outer layers expand, eventually transforming the Sun into a red giant. It is calculated that the Sun will become sufficiently large to engulf the current orbits of Mercury and Venus, and render Earth uninhabitable – but not for about five billion years. After this, it will shed its outer layers and become a dense type of cooling star known as a white dwarf, and no longer produce energy by fusion, but still glow and give off heat from its previous fusion.

The enormous effect of the Sun on Earth has been recognized since prehistoric times. The Sun was thought of by some cultures as a deity. The synodic rotation of Earth and its orbit around the Sun are the basis of some solar calendars. The predominant calendar in use today is the Gregorian calendar which is based upon the standard 16th-century interpretation of the Sun's observed movement as actual movement. [23]

## Etymology

The English word sun developed from Old English sunne. Cognates appear in other Germanic languages, including West Frisian sinne, Dutch zon, Low German Sünn, Standard German Sonne, Bavarian Sunna, Old Norse sunna, and Gothic sunnō. All these words stem from Proto-Germanic *sunnōn. [24] [25] This is ultimately related to the word for sun in other branches of the Indo-European language family, though in most cases a nominative stem with an l is found, rather than the genitive stem in n, as for example in Latin sōl, ancient Greek ἥλιος (hēlios), Welsh haul and Russian солнце (solntse; pronounced sontse), as well as (with *l > r) Sanskrit स्वर (svár) and Persian خور (xvar). Indeed, the l-stem survived in Proto-Germanic as well, as *sōwelan, which gave rise to Gothic sauil (alongside sunnō) and Old Norse prosaic sól (alongside poetic sunna), and through it the words for sun in the modern Scandinavian languages: Swedish and Danish solen, Icelandic sólin, etc. [25]

The principal adjectives for the Sun in English are sunny for sunlight and, in technical contexts, solar (), [3] from Latin sol [26] – the latter found in terms such as solar day, solar eclipse and Solar System (occasionally Sol system). From the Greek helios comes the rare adjective heliac (). [27] In English, the Greek and Latin words occur in poetry as personifications of the Sun, Helios () and Sol (), [2] [1] while in science fiction Sol may be used as a name for the Sun to distinguish it from other stars. The term sol with a lower-case s is used by planetary astronomers for the duration of a solar day on another planet such as Mars. [28]

The English weekday name Sunday stems from Old English Sunnandæg "sun's day", a Germanic interpretation of the Latin phrase diēs sōlis, itself a translation of the ancient Greek ἡμέρα ἡλίου ( hēmera hēliou) 'day of the sun'. [29] The astronomical symbol for the Sun is a circle with a center dot, . It is used for such units as M (Solar mass), R (Solar radius) and L (Solar luminosity).

## General characteristics

The Sun is a G-type main-sequence star that constitutes about 99.86% of the mass of the Solar System. The Sun has an absolute magnitude of +4.83, estimated to be brighter than about 85% of the stars in the Milky Way, most of which are red dwarfs. [30] [31] The Sun is a Population I, or heavy-element-rich, [lower-alpha 2] star. [32] The formation of the Sun may have been triggered by shockwaves from one or more nearby supernovae. [33] This is suggested by a high abundance of heavy elements in the Solar System, such as gold and uranium, relative to the abundances of these elements in so-called Population II, heavy-element-poor, stars. The heavy elements could most plausibly have been produced by endothermic nuclear reactions during a supernova, or by transmutation through neutron absorption within a massive second-generation star. [32]

The Sun is by far the brightest object in the Earth's sky, with an apparent magnitude of −26.74. [34] [35] This is about 13 billion times brighter than the next brightest star, Sirius, which has an apparent magnitude of −1.46. One astronomical unit (about 150,000,000 km; 93,000,000 mi) is defined as the mean distance of the Sun's center to Earth's center, though the distance varies as Earth moves from perihelion in January to aphelion in July. [36] The distances can vary between 147,098,074 km (perihelion) and 152,097,701 km (aphelion), and extreme values can range from 147,083,346 km to 152,112,126 km. [37] At its average distance, light travels from the Sun's horizon to Earth's horizon in about 8 minutes and 20 seconds, [38] while light from the closest points of the Sun and Earth takes about two seconds less. The energy of this sunlight supports almost all life [lower-alpha 3] on Earth by photosynthesis, [39] and drives Earth's climate and weather.

The Sun does not have a definite boundary, but its density decreases exponentially with increasing height above the photosphere. [40] For the purpose of measurement, the Sun's radius is considered to be the distance from its center to the edge of the photosphere, the apparent visible surface of the Sun. [41] By this measure, the Sun is a near-perfect sphere with an oblateness estimated at 9 millionths, [42] which means that its polar diameter differs from its equatorial diameter by only 10 kilometers (6.2 mi). [43] The tidal effect of the planets is weak and does not significantly affect the shape of the Sun. [44] The Sun rotates faster at its equator than at its poles. This differential rotation is caused by convective motion due to heat transport and the Coriolis force due to the Sun's rotation. In a frame of reference defined by the stars, the rotational period is approximately 25.6 days at the equator and 33.5 days at the poles. Viewed from Earth as it orbits the Sun, the apparent rotational period of the Sun at its equator is about 28 days. [45] Viewed from a vantage point above its north pole, the Sun rotates counterclockwise around its axis of spin. [lower-alpha 4] [46]

## Composition

The Sun is composed primarily of the chemical elements hydrogen and helium. At this time in the Sun's life, they account for 74.9% and 23.8%, respectively, of the mass of the Sun in the photosphere. [47] All heavier elements, called metals in astronomy, account for less than 2% of the mass, with oxygen (roughly 1% of the Sun's mass), carbon (0.3%), neon (0.2%), and iron (0.2%) being the most abundant. [48]

The Sun's original chemical composition was inherited from the interstellar medium out of which it formed. Originally it would have contained about 71.1% hydrogen, 27.4% helium, and 1.5% heavier elements. [47] The hydrogen and most of the helium in the Sun would have been produced by Big Bang nucleosynthesis in the first 20 minutes of the universe, and the heavier elements were produced by previous generations of stars before the Sun was formed, and spread into the interstellar medium during the final stages of stellar life and by events such as supernovae. [49]

Since the Sun formed, the main fusion process has involved fusing hydrogen into helium. Over the past 4.6 billion years, the amount of helium and its location within the Sun has gradually changed. Within the core, the proportion of helium has increased from about 24% to about 60% due to fusion, and some of the helium and heavy elements have settled from the photosphere towards the center of the Sun because of gravity. The proportions of heavier elements is unchanged. Heat is transferred outward from the Sun's core by radiation rather than by convection (see Radiative zone below), so the fusion products are not lifted outward by heat; they remain in the core [50] and gradually an inner core of helium has begun to form that cannot be fused because presently the Sun's core is not hot or dense enough to fuse helium. In the current photosphere, the helium fraction is reduced, and the metallicity is only 84% of what it was in the protostellar phase (before nuclear fusion in the core started). In the future, helium will continue to accumulate in the core, and in about 5 billion years this gradual build-up will eventually cause the Sun to exit the main sequence and become a red giant. [51]

The chemical composition of the photosphere is normally considered representative of the composition of the primordial Solar System. [52] The solar heavy-element abundances described above are typically measured both using spectroscopy of the Sun's photosphere and by measuring abundances in meteorites that have never been heated to melting temperatures. These meteorites are thought to retain the composition of the protostellar Sun and are thus not affected by the settling of heavy elements. The two methods generally agree well. [21]

## Structure and fusion

### Core

The core of the Sun extends from the center to about 20–25% of the solar radius. [53] It has a density of up to 150 g/cm3 [54] [55] (about 150 times the density of water) and a temperature of close to 15.7 million Kelvin (K). [55] By contrast, the Sun's surface temperature is approximately 5800 K. Recent analysis of SOHO mission data favors a faster rotation rate in the core than in the radiative zone above. [53] Through most of the Sun's life, energy has been produced by nuclear fusion in the core region through the proton–proton chain; this process converts hydrogen into helium. [56] Currently, only 0.8% of the energy generated in the Sun comes from another sequence of fusion reactions called the CNO cycle, though this proportion is expected to increase as the Sun becomes older and more luminous. [57] [58]

The core is the only region in the Sun that produces an appreciable amount of thermal energy through fusion; 99% of the power is generated within 24% of the Sun's radius, and by 30% of the radius, fusion has stopped nearly entirely. The remainder of the Sun is heated by this energy as it is transferred outwards through many successive layers, finally to the solar photosphere where it escapes into space through radiation (photons) or advection (massive particles). [59] [60]

The proton–proton chain occurs around 9.2×1037 times each second in the core, converting about 3.7×1038 protons into alpha particles (helium nuclei) every second (out of a total of ~8.9×1056 free protons in the Sun), or about 6.2×1011 kg/s. However, each proton (on average) takes around 9 billion years to fuse with one another using the PP chain. [59] Fusing four free protons (hydrogen nuclei) into a single alpha particle (helium nucleus) releases around 0.7% of the fused mass as energy, [61] so the Sun releases energy at the mass–energy conversion rate of 4.26 million metric tons per second (which requires 600 metric megatons of hydrogen [62] ), for 384.6  yottawatts (3.846×1026 W), [5] or 9.192×1010  megatons of TNT per second. The large power output of the Sun is mainly due to the huge size and density of its core (compared to Earth and objects on Earth), with only a fairly small amount of power being generated per cubic metre. Theoretical models of the Sun's interior indicate a maximum power density, or energy production, of approximately 276.5 watts per cubic metre at the center of the core, [63] which is about the same power density inside a compost pile. [64] [lower-alpha 5]

The fusion rate in the core is in a self-correcting equilibrium: a slightly higher rate of fusion would cause the core to heat up more and expand slightly against the weight of the outer layers, reducing the density and hence the fusion rate and correcting the perturbation; and a slightly lower rate would cause the core to cool and shrink slightly, increasing the density and increasing the fusion rate and again reverting it to its present rate. [65] [66]

### Tachocline

The radiative zone and the convective zone are separated by a transition layer, the tachocline. This is a region where the sharp regime change between the uniform rotation of the radiative zone and the differential rotation of the convection zone results in a large shear between the two—a condition where successive horizontal layers slide past one another. [68] Presently, it is hypothesized (see Solar dynamo) that a magnetic dynamo within this layer generates the Sun's magnetic field. [55]

### Convective zone

The Sun's convection zone extends from 0.7 solar radii (500,000 km) to near the surface. In this layer, the solar plasma is not dense enough or hot enough to transfer the heat energy of the interior outward via radiation. Instead, the density of the plasma is low enough to allow convective currents to develop and move the Sun's energy outward towards its surface. Material heated at the tachocline picks up heat and expands, thereby reducing its density and allowing it to rise. As a result, an orderly motion of the mass develops into thermal cells that carry the majority of the heat outward to the Sun's photosphere above. Once the material diffusively and radiatively cools just beneath the photospheric surface, its density increases, and it sinks to the base of the convection zone, where it again picks up heat from the top of the radiative zone and the convective cycle continues. At the photosphere, the temperature has dropped to 5,700 K (350-fold) and the density to only 0.2 g/m3 (about 1/10,000 the density of air at sea level, and 1 millionth that of the inner layer of the convective zone). [55]

The thermal columns of the convection zone form an imprint on the surface of the Sun giving it a granular appearance called the solar granulation at the smallest scale and supergranulation at larger scales. Turbulent convection in this outer part of the solar interior sustains "small-scale" dynamo action over the near-surface volume of the Sun. [55] The Sun's thermal columns are Bénard cells and take the shape of roughly hexagonal prisms. [69]

### Photosphere

The visible surface of the Sun, the photosphere, is the layer below which the Sun becomes opaque to visible light. [70] Photons produced in this layer escape the Sun through the transparent solar atmosphere above it and become solar radiation, sunlight. The change in opacity is due to the decreasing amount of H ions, which absorb visible light easily. [70] Conversely, the visible light we see is produced as electrons react with hydrogen atoms to produce H ions. [71] [72]

The photosphere is tens to hundreds of kilometers thick, and is slightly less opaque than air on Earth. Because the upper part of the photosphere is cooler than the lower part, an image of the Sun appears brighter in the center than on the edge or limb of the solar disk, in a phenomenon known as limb darkening. [70] The spectrum of sunlight has approximately the spectrum of a black-body radiating at 5,777 K (5,504 °C; 9,939 °F), interspersed with atomic absorption lines from the tenuous layers above the photosphere. The photosphere has a particle density of ~1023 m−3 (about 0.37% of the particle number per volume of Earth's atmosphere at sea level). The photosphere is not fully ionized—the extent of ionization is about 3%, leaving almost all of the hydrogen in atomic form. [73]

During early studies of the optical spectrum of the photosphere, some absorption lines were found that did not correspond to any chemical elements then known on Earth. In 1868, Norman Lockyer hypothesized that these absorption lines were caused by a new element that he dubbed helium, after the Greek Sun god Helios. Twenty-five years later, helium was isolated on Earth. [74]

### Atmosphere

During a total solar eclipse, when the disk of the Sun is covered by that of the Moon, parts of the Sun's surrounding atmosphere can be seen. It is composed of four distinct parts: the chromosphere, the transition region, the corona and the heliosphere.

The coolest layer of the Sun is a temperature minimum region extending to about 500 km above the photosphere, and has a temperature of about 4,100  K . [70] This part of the Sun is cool enough to allow the existence of simple molecules such as carbon monoxide and water, which can be detected via their absorption spectra. [75]

The chromosphere, transition region, and corona are much hotter than the surface of the Sun. [70] The reason is not well understood, but evidence suggests that Alfvén waves may have enough energy to heat the corona. [76]

Above the temperature minimum layer is a layer about 2,000 km thick, dominated by a spectrum of emission and absorption lines. [70] It is called the chromosphere from the Greek root chroma, meaning color, because the chromosphere is visible as a colored flash at the beginning and end of total solar eclipses. [67] The temperature of the chromosphere increases gradually with altitude, ranging up to around 20,000 K near the top. [70] In the upper part of the chromosphere helium becomes partially ionized. [77]

Above the chromosphere, in a thin (about 200 km) transition region, the temperature rises rapidly from around 20,000 K in the upper chromosphere to coronal temperatures closer to 1,000,000 K. [78] The temperature increase is facilitated by the full ionization of helium in the transition region, which significantly reduces radiative cooling of the plasma. [77] The transition region does not occur at a well-defined altitude. Rather, it forms a kind of nimbus around chromospheric features such as spicules and filaments, and is in constant, chaotic motion. [67] The transition region is not easily visible from Earth's surface, but is readily observable from space by instruments sensitive to the extreme ultraviolet portion of the spectrum. [79]

The corona is the next layer of the Sun. The low corona, near the surface of the Sun, has a particle density around 1015 m−3 to 1016 m−3. [77] [lower-alpha 6] The average temperature of the corona and solar wind is about 1,000,000–2,000,000 K; however, in the hottest regions it is 8,000,000–20,000,000 K. [78] Although no complete theory yet exists to account for the temperature of the corona, at least some of its heat is known to be from magnetic reconnection. [78] [80] The corona is the extended atmosphere of the Sun, which has a volume much larger than the volume enclosed by the Sun's photosphere. A flow of plasma outward from the Sun into interplanetary space is the solar wind. [80]

The heliosphere, the tenuous outermost atmosphere of the Sun, is filled with the solar wind plasma. This outermost layer of the Sun is defined to begin at the distance where the flow of the solar wind becomes superalfvénic—that is, where the flow becomes faster than the speed of Alfvén waves, [81] at approximately 20 solar radii (0.1 AU). Turbulence and dynamic forces in the heliosphere cannot affect the shape of the solar corona within, because the information can only travel at the speed of Alfvén waves. The solar wind travels outward continuously through the heliosphere, [82] [83] forming the solar magnetic field into a spiral shape, [80] until it impacts the heliopause more than 50 AU from the Sun. In December 2004, the Voyager 1 probe passed through a shock front that is thought to be part of the heliopause. [84] In late 2012 Voyager 1 recorded a marked increase in cosmic ray collisions and a sharp drop in lower energy particles from the solar wind, which suggested that the probe had passed through the heliopause and entered the interstellar medium, [85] and indeed did so August 25, 2012 at approximately 122 astronomical units from the Sun. [86] The heliosphere has a heliotail which stretches out behind it due to the Sun's movement. [87]

On April 28, 2021, during its eighth flyby of the Sun, NASA's Parker Solar Probe encountered the specific magnetic and particle conditions at 18.8 solar radii that indicated that it penetrated the Alfvén surface, the boundary separating the corona from the solar wind defined as where the coronal plasma's Alfvén speed and the large-scale solar wind speed are equal. [88] [89] The probe measured the solar wind plasma environment with its FIELDS and SWEAP instruments. [90] This event was described by NASA as "touching the Sun". [88] During the flyby, Parker Solar Probe passed into and out of the corona several times. This proved the predictions that the Alfvén critical surface isn't shaped like a smooth ball, but has spikes and valleys that wrinkle its surface. [88]

### Sunlight and neutrinos

The Sun emits light across the visible spectrum, so its color is white, with a CIE color-space index near (0.3, 0.3), when viewed from space or when the Sun is high in the sky. The Solar radiance per wavelength peaks in the green portion of the spectrum when viewed from space. [91] [92] When the Sun is very low in the sky, atmospheric scattering renders the Sun yellow, red, orange, or magenta, and in rare occasions even green or blue. Despite its typical whiteness (white sunrays, white ambient light, white illumination of the Moon, etc.), some cultures mentally picture the Sun as yellow and some even red; the reasons for this are cultural and exact ones are the subject of debate. [93] The Sun is a G2V star, with G2 indicating its surface temperature of approximately 5,778 K (5,505 °C; 9,941 °F), and V that it, like most stars, is a main-sequence star. [59] [94]

The solar constant is the amount of power that the Sun deposits per unit area that is directly exposed to sunlight. The solar constant is equal to approximately 1,368 W/m2 (watts per square meter) at a distance of one astronomical unit (AU) from the Sun (that is, on or near Earth). [95] Sunlight on the surface of Earth is attenuated by Earth's atmosphere, so that less power arrives at the surface (closer to 1,000 W/m2) in clear conditions when the Sun is near the zenith. [96] Sunlight at the top of Earth's atmosphere is composed (by total energy) of about 50% infrared light, 40% visible light, and 10% ultraviolet light. [97] The atmosphere in particular filters out over 70% of solar ultraviolet, especially at the shorter wavelengths. [98] Solar ultraviolet radiation ionizes Earth's dayside upper atmosphere, creating the electrically conducting ionosphere. [99]

Ultraviolet light from the Sun has antiseptic properties and can be used to sanitize tools and water. It also causes sunburn, and has other biological effects such as the production of vitamin D and sun tanning. It is also the main cause of skin cancer. Ultraviolet light is strongly attenuated by Earth's ozone layer, so that the amount of UV varies greatly with latitude and has been partially responsible for many biological adaptations, including variations in human skin color in different regions of the Earth. [100]

High-energy gamma ray photons initially released with fusion reactions in the core are almost immediately absorbed by the solar plasma of the radiative zone, usually after traveling only a few millimeters. Re-emission happens in a random direction and usually at slightly lower energy. With this sequence of emissions and absorptions, it takes a long time for radiation to reach the Sun's surface. Estimates of the photon travel time range between 10,000 and 170,000 years. [101] In contrast, it takes only 2.3 seconds for the neutrinos, which account for about 2% of the total energy production of the Sun, to reach the surface. Because energy transport in the Sun is a process that involves photons in thermodynamic equilibrium with matter, the time scale of energy transport in the Sun is longer, on the order of 30,000,000 years. This is the time it would take the Sun to return to a stable state if the rate of energy generation in its core were suddenly changed. [102]

Neutrinos are also released by the fusion reactions in the core, but, unlike photons, they rarely interact with matter, so almost all are able to escape the Sun immediately. For many years measurements of the number of neutrinos produced in the Sun were lower than theories predicted by a factor of 3. This discrepancy was resolved in 2001 through the discovery of the effects of neutrino oscillation: the Sun emits the number of neutrinos predicted by the theory, but neutrino detectors were missing 23 of them because the neutrinos had changed flavor by the time they were detected. [103]

## Magnetic activity

The Sun has a stellar magnetic field that varies across its surface. Its polar field is 1–2 gauss (0.0001–0.0002  T ), whereas the field is typically 3,000 gauss (0.3 T) in features on the Sun called sunspots and 10–100 gauss (0.001–0.01 T) in solar prominences. [5] The magnetic field varies in time and location. The quasi-periodic 11-year solar cycle is the most prominent variation in which the number and size of sunspots waxes and wanes. [104] [105] [106]

The solar magnetic field extends well beyond the Sun itself. The electrically conducting solar wind plasma carries the Sun's magnetic field into space, forming what is called the interplanetary magnetic field. [80] In an approximation known as ideal magnetohydrodynamics, plasma particles only move along the magnetic field lines. As a result, the outward-flowing solar wind stretches the interplanetary magnetic field outward, forcing it into a roughly radial structure. For a simple dipolar solar magnetic field, with opposite hemispherical polarities on either side of the solar magnetic equator, a thin current sheet is formed in the solar wind. [80]

At great distances, the rotation of the Sun twists the dipolar magnetic field and corresponding current sheet into an Archimedean spiral structure called the Parker spiral. [80] The interplanetary magnetic field is much stronger than the dipole component of the solar magnetic field. The Sun's dipole magnetic field of 50–400  μT (at the photosphere) reduces with the inverse-cube of the distance, leading to a predicted magnetic field of 0.1 nT at the distance of Earth. However, according to spacecraft observations the interplanetary field at Earth's location is around 5 nT, about a hundred times greater. [107] The difference is due to magnetic fields generated by electrical currents in the plasma surrounding the Sun.

### Sunspot

Sunspots are visible as dark patches on the Sun's photosphere and correspond to concentrations of magnetic field where the convective transport of heat is inhibited from the solar interior to the surface. As a result, sunspots are slightly cooler than the surrounding photosphere, so they appear dark. At a typical solar minimum, few sunspots are visible, and occasionally none can be seen at all. Those that do appear are at high solar latitudes. As the solar cycle progresses towards its maximum, sunspots tend to form closer to the solar equator, a phenomenon known as Spörer's law. The largest sunspots can be tens of thousands of kilometers across. [108]

An 11-year sunspot cycle is half of a 22-year Babcock–Leighton dynamo cycle, which corresponds to an oscillatory exchange of energy between toroidal and poloidal solar magnetic fields. At solar-cycle maximum, the external poloidal dipolar magnetic field is near its dynamo-cycle minimum strength, but an internal toroidal quadrupolar field, generated through differential rotation within the tachocline, is near its maximum strength. At this point in the dynamo cycle, buoyant upwelling within the convective zone forces emergence of the toroidal magnetic field through the photosphere, giving rise to pairs of sunspots, roughly aligned east–west and having footprints with opposite magnetic polarities. The magnetic polarity of sunspot pairs alternates every solar cycle, a phenomenon described by Hale's law. [109] [110]

During the solar cycle's declining phase, energy shifts from the internal toroidal magnetic field to the external poloidal field, and sunspots diminish in number and size. At solar-cycle minimum, the toroidal field is, correspondingly, at minimum strength, sunspots are relatively rare, and the poloidal field is at its maximum strength. With the rise of the next 11-year sunspot cycle, differential rotation shifts magnetic energy back from the poloidal to the toroidal field, but with a polarity that is opposite to the previous cycle. The process carries on continuously, and in an idealized, simplified scenario, each 11-year sunspot cycle corresponds to a change, then, in the overall polarity of the Sun's large-scale magnetic field. [111] [112]

### Solar activity

The Sun's magnetic field leads to many effects that are collectively called solar activity. Solar flares and coronal-mass ejections tend to occur at sunspot groups. Slowly changing high-speed streams of solar wind are emitted from coronal holes at the photospheric surface. Both coronal-mass ejections and high-speed streams of solar wind carry plasma and interplanetary magnetic field outward into the Solar System. [113] The effects of solar activity on Earth include auroras at moderate to high latitudes and the disruption of radio communications and electric power. Solar activity is thought to have played a large role in the formation and evolution of the Solar System.

Long-term secular change in sunspot number is thought, by some scientists, to be correlated with long-term change in solar irradiance, [114] which, in turn, might influence Earth's long-term climate. [115] The solar cycle influences space weather conditions, including those surrounding Earth. For example, in the 17th century, the solar cycle appeared to have stopped entirely for several decades; few sunspots were observed during a period known as the Maunder minimum. This coincided in time with the era of the Little Ice Age, when Europe experienced unusually cold temperatures. [116] Earlier extended minima have been discovered through analysis of tree rings and appear to have coincided with lower-than-average global temperatures. [117]

In December 2019, a new type of solar magnetic explosion was observed, known as forced magnetic reconnection. Previously, in a process called spontaneous magnetic reconnection, it was observed that the solar magnetic field lines diverge explosively and then converge again instantaneously. Forced Magnetic Reconnection was similar, but it was triggered by an explosion in the corona. [118]

## Life phases

The Sun today is roughly halfway through the most stable part of its life. It has not changed dramatically for over four billion [lower-alpha 1] years and will remain fairly stable for more than five billion more. However, after hydrogen fusion in its core has stopped, the Sun will undergo dramatic changes, both internally and externally. It is more massive than 71 of 75 other stars within 5 pc, [119] or in the top ~5 percent.

### Formation

The Sun formed about 4.6 billion years ago from the collapse of part of a giant molecular cloud that consisted mostly of hydrogen and helium and that probably gave birth to many other stars. [120] This age is estimated using computer models of stellar evolution and through nucleocosmochronology. [14] The result is consistent with the radiometric date of the oldest Solar System material, at 4.567 billion years ago. [121] [122] Studies of ancient meteorites reveal traces of stable daughter nuclei of short-lived isotopes, such as iron-60, that form only in exploding, short-lived stars. This indicates that one or more supernovae must have occurred near the location where the Sun formed. A shock wave from a nearby supernova would have triggered the formation of the Sun by compressing the matter within the molecular cloud and causing certain regions to collapse under their own gravity. [123] As one fragment of the cloud collapsed it also began to rotate due to conservation of angular momentum and heat up with the increasing pressure. Much of the mass became concentrated in the center, whereas the rest flattened out into a disk that would become the planets and other Solar System bodies. Gravity and pressure within the core of the cloud generated a lot of heat as it accumulated more matter from the surrounding disk, eventually triggering nuclear fusion.

HD 162826 and HD 186302 are hypothesized stellar siblings of the Sun, having formed in the same molecular cloud.

### Main sequence

The Sun is about halfway through its main-sequence stage, during which nuclear fusion reactions in its core fuse hydrogen into helium. Each second, more than four million tonnes of matter are converted into energy within the Sun's core, producing neutrinos and solar radiation. At this rate, the Sun has so far converted around 100 times the mass of Earth into energy, about 0.03% of the total mass of the Sun. The Sun will spend a total of approximately 10 to 11  billion years as a main-sequence star before the red giant phase of the sun. [124] At the 8 billion year mark, the sun will be at its hottest point according to the ESA's Gaia space observatory mission in 2022. [125]

The Sun is gradually becoming hotter in its core, hotter at the surface, larger in radius, and more luminous during its time on the main sequence: since the beginning of its main sequence life, it has expanded in radius by 15% and the surface has increased in temperature from 5,620 K (5,350 °C; 9,660 °F) to 5,777 K (5,504 °C; 9,939 °F), resulting in a 48% increase in luminosity from 0.677 solar luminosities to its present-day 1.0 solar luminosity. This occurs because the helium atoms in the core have a higher mean molecular weight than the hydrogen atoms that were fused, resulting in less thermal pressure. The core is therefore shrinking, allowing the outer layers of the Sun to move closer to the center, releasing gravitational potential energy. According to the virial theorem, half this released gravitational energy goes into heating, which leads to a gradual increase in the rate at which fusion occurs and thus an increase in the luminosity. This process speeds up as the core gradually becomes denser. [126] At present, it is increasing in brightness by about 1% every 100 million years. It will take at least 1 billion years from now to deplete liquid water from the Earth from such increase. [127] After that, the Earth will cease to be able to support complex, multicellular life and the last remaining multicellular organisms on the planet will suffer a final, complete mass extinction. [128]

### After core hydrogen exhaustion

The Sun does not have enough mass to explode as a supernova. Instead, when it runs out of hydrogen in the core in approximately 5 billion years, core hydrogen fusion will stop, and there will be nothing to prevent the core from contracting. The release of gravitational potential energy will cause the luminosity of the Sun to increase, ending the main sequence phase and leading the Sun to expand over the next billion years: first into a subgiant, and then into a red giant. [126] [129] [130] The heating due to gravitational contraction will also lead to hydrogen fusion in a shell just outside the core, where unfused hydrogen remains, contributing to the increased luminosity, which will eventually reach more than 1,000 times its present luminosity. [126] When the Sun enters its red-giant branch (RGB) phase, it will engulf Mercury and (likely) Venus, reaching about 0.75 AU (110 million km; 70 million mi). [130] [131] The Sun will spend around a billion years in the RGB and lose around a third of its mass. [130]

After the red-giant branch, the Sun has approximately 120 million years of active life left, but much happens. First, the core (full of degenerate helium) ignites violently in the helium flash; it is estimated that 6% of the core—itself 40% of the Sun's mass—will be converted into carbon within a matter of minutes through the triple-alpha process. [132] The Sun then shrinks to around 10 times its current size and 50 times the luminosity, with a temperature a little lower than today. It will then have reached the red clump or horizontal branch, but a star of the Sun's metallicity does not evolve blueward along the horizontal branch. Instead, it just becomes moderately larger and more luminous over about 100 million years as it continues to react helium in the core. [130]

When the helium is exhausted, the Sun will repeat the expansion it followed when the hydrogen in the core was exhausted. This time, however, it all happens faster, and the Sun becomes larger and more luminous, engulfing Venus if it has not already. This is the asymptotic-giant-branch phase, and the Sun is alternately reacting hydrogen in a shell or helium in a deeper shell. After about 20 million years on the early asymptotic giant branch, the Sun becomes increasingly unstable, with rapid mass loss and thermal pulses that increase the size and luminosity for a few hundred years every 100,000 years or so. The thermal pulses become larger each time, with the later pulses pushing the luminosity to as much as 5,000 times the current level and the radius to over 1 AU (150 million km; 93 million mi). [133]

According to a 2008 model, Earth's orbit will have initially expanded to at most 1.5 AU (220 million km; 140 million mi) due to the Sun's loss of mass as a red giant. However, Earth's orbit will later start shrinking due to tidal forces (and, eventually, drag from the lower chromosphere) so that it is engulfed by the Sun during the tip of the red-giant branch phase, 3.8 and 1 million years after Mercury and Venus have respectively suffered the same fate. Models vary depending on the rate and timing of mass loss. Models that have higher mass loss on the red-giant branch produce smaller, less luminous stars at the tip of the asymptotic giant branch, perhaps only 2,000 times the luminosity and less than 200 times the radius. [130] For the Sun, four thermal pulses are predicted before it completely loses its outer envelope and starts to make a planetary nebula. By the end of that phase—lasting approximately 500,000 years—the Sun will only have about half of its current mass.

The post-asymptotic-giant-branch evolution is even faster. The luminosity stays approximately constant as the temperature increases, with the ejected half of the Sun's mass becoming ionized into a planetary nebula as the exposed core reaches 30,000 K (29,700 °C; 53,500 °F), as if it is in a sort of blue loop. The final naked core, a white dwarf, will have a temperature of over 100,000 K (100,000 °C; 180,000 °F), and contain an estimated 54.05% of the Sun's present-day mass. [130] The planetary nebula will disperse in about 10,000 years, but the white dwarf will survive for trillions of years before fading to a hypothetical black dwarf. [134] [135]

## Motion and location

### Solar System

The Sun has eight known planets orbiting around it. This includes four terrestrial planets (Mercury, Venus, Earth, and Mars), two gas giants (Jupiter and Saturn), and two ice giants (Uranus and Neptune). The Solar System also has nine bodies generally considered as dwarf planets and some more candidates, an asteroid belt, numerous comets, and a large number of icy bodies which lie beyond the orbit of Neptune. Six of the planets and many smaller bodies also have their own natural satellites: in particular, the satellite systems of Jupiter, Saturn, and Uranus are in some ways like miniature versions of the Sun's system. [136]

The Sun is moved by the gravitational pull of the planets. The center of the Sun is always within 2.2 solar radii of the barycenter. This motion of the Sun is mainly due to Jupiter, Saturn, Uranus, and Neptune. For some periods of several decades, the motion is rather regular, forming a trefoil pattern, whereas between these periods it appears more chaotic. [137] After 179 years (nine times the synodic period of Jupiter and Saturn), the pattern more or less repeats, but rotated by about 24°. [138] The orbits of the inner planets, including of the Earth, are similarly displaced by the same gravitational forces, so the movement of the Sun has little effect on the relative positions of the Earth and the Sun or on solar irradiance on the Earth as a function of time. [139]

### Celestial neighbourhood

The Solar System is surrounded by the Local Interstellar Cloud, although it is not clear if it is embedded in the Local Interstellar Cloud or if it lies just outside the cloud's edge. [140] [141] Multiple other interstellar clouds also exist in the region within 300 light-years of the Sun, known as the Local Bubble. [141] The latter feature is an hourglass-shaped cavity or superbubble in the interstellar medium roughly 300 light-years across. The bubble is suffused with high-temperature plasma, suggesting that it may be the product of several recent supernovae. [142]

The Local Bubble is a small superbubble compared to the neighbouring wider Radcliffe Wave and Split linear structures (formerly Gould Belt), each of which are some thousands of light-years in length. [143] All these structures are part of the Orion Arm, which contains most of the stars in the Milky Way that are visible to the unaided eye. The density of all matter in the local neighborhood is 0.097±0.013  M ·pc−3. [144]

Within ten light-years of the Sun there are relatively few stars, the closest being the triple star system Alpha Centauri, which is about 4.4 light-years away and may be in the Local Bubble's G-Cloud. [145] Alpha Centauri A and B are a closely tied pair of Sun-like stars, whereas the closest star to Earth, the small red dwarf Proxima Centauri, orbits the pair at a distance of 0.2 light-year. In 2016, a potentially habitable exoplanet was found to be orbiting Proxima Centauri, called Proxima Centauri b, the closest confirmed exoplanet to the Sun. [146]

The next closest known fusors to the Sun are the red dwarfs Barnard's Star (at 5.9 ly), Wolf 359 (7.8 ly), and Lalande 21185 (8.3 ly). [147] The nearest brown dwarfs belong to the binary Luhman 16 system (6.6 ly), and the closest known rogue or free-floating planetary-mass object at less than 10 Jupiter masses is the sub-brown dwarf WISE 0855−0714 (7.4 ly). [148]

Just beyond at 8.6 ly lies Sirius, the brightest star in Earth's night sky, with roughly twice the Sun's mass, orbited by the closest white dwarf to Earth, Sirius B. Other stars within ten light-years are the binary red-dwarf system Luyten 726-8 (8.7 ly) and the solitary red dwarf Ross 154 (9.7 ly). [149] [150] The closest solitary Sun-like star to the Solar System is Tau Ceti at 11.9 light-years. It has roughly 80% of the Sun's mass but only about half of its luminosity. [151]

The nearest and unaided-visible group of stars beyond the immediate celestial neighbourhood is the Ursa Major Moving Group at roughly 80 light-years, which is within the Local Bubble, like the nearest as well as unaided-visible star cluster the Hyades, which lie at its edge. The closest star-forming regions are the Corona Australis Molecular Cloud, the Rho Ophiuchi cloud complex and the Taurus Molecular Cloud; the latter lies just beyond the Local Bubble and is part of the Radcliffe wave. [152]

### Galactic context

Diagram of the Milky Way with the position of the Solar System marked by a yellow arrow and a red dot in the Orion Arm, the dot roughly covering the large surrounding celestial area dominated by the Radcliffe Wave and Split linear structures (formerly Gould Belt). [143]

The Solar System is located in the Milky Way, a barred spiral galaxy with a diameter of about 100,000 light-years containing more than 100 billion stars. [153] The Sun resides in one of the Milky Way's outer spiral arms, known as the Orion–Cygnus Arm or Local Spur. [154] The Sun lies about 26,660 light-years from the Galactic Center, [155] and its speed around the center of the Milky Way is about 220 km/s, so that it completes one revolution every 240 million years. [153] This revolution is known as the Solar System's galactic year. [156] The solar apex, the direction of the Sun's path through interstellar space, is near the constellation Hercules in the direction of the current location of the bright star Vega. [157] The plane of the ecliptic lies at an angle of about 60° to the galactic plane. [lower-alpha 7]

The Solar System's location in the Milky Way is a factor in the evolutionary history of life on Earth. Its orbit is close to circular, and orbits near the Sun are at roughly the same speed as that of the spiral arms. [159] [160] Therefore, the Sun passes through arms only rarely. Because spiral arms are home to a far larger concentration of supernovae, gravitational instabilities, and radiation that could disrupt the Solar System, this has given Earth long periods of stability for life to evolve. [159] However, the changing position of the Solar System relative to other parts of the Milky Way could explain periodic extinction events on Earth, according to the Shiva hypothesis or related theories, but this remains controversial. [161] [162]

The Solar System lies well outside the star-crowded environs of the galactic centre. Near the centre, gravitational tugs from nearby stars could perturb bodies in the Oort cloud and send many comets into the inner Solar System, producing collisions with potentially catastrophic implications for life on Earth. The intense radiation of the galactic centre could also interfere with the development of complex life. [159] Stellar flybys that pass within 0.8 light-years of the Sun occur roughly once every 100,000 years. The closest well-measured approach was Scholz's Star, which approached to 52+23
−14
kAU
of the Sun some 70+15
−10
kya
, likely passing through the outer Oort cloud. [163]

## Observational history

### Early understanding

The Sun has been an object of veneration in many cultures throughout human history. Humanity's most fundamental understanding of the Sun is as the luminous disk in the sky, whose presence above the horizon causes day and whose absence causes night. In many prehistoric and ancient cultures, the Sun was thought to be a solar deity or other supernatural entity. The Sun has played an important part in many world religions, as described in a later section.

In the early first millennium BC, Babylonian astronomers observed that the Sun's motion along the ecliptic is not uniform, though they did not know why; it is today known that this is due to the movement of Earth in an elliptic orbit around the Sun, with Earth moving faster when it is nearer to the Sun at perihelion and moving slower when it is farther away at aphelion. [164]

One of the first people to offer a scientific or philosophical explanation for the Sun was the Greek philosopher Anaxagoras. He reasoned that it was not the chariot of Helios, but instead a giant flaming ball of metal even larger than the land of the Peloponnesus and that the Moon reflected the light of the Sun. [165] For teaching this heresy, he was imprisoned by the authorities and sentenced to death, though he was later released through the intervention of Pericles. Eratosthenes estimated the distance between Earth and the Sun in the third century BC as "of stadia myriads 400 and 80000", the translation of which is ambiguous, implying either 4,080,000 stadia (755,000 km) or 804,000,000 stadia (148 to 153 million kilometers or 0.99 to 1.02 AU); the latter value is correct to within a few percent. In the first century AD, Ptolemy estimated the distance as 1,210 times the radius of Earth, approximately 7.71 million kilometers (0.0515 AU). [166]

The theory that the Sun is the center around which the planets orbit was first proposed by the ancient Greek Aristarchus of Samos in the third century BC, and later adopted by Seleucus of Seleucia (see Heliocentrism). This view was developed in a more detailed mathematical model of a heliocentric system in the 16th century by Nicolaus Copernicus.

### Development of scientific understanding

Observations of sunspots were recorded during the Han Dynasty (206 BC–AD 220) by Chinese astronomers, who maintained records of these observations for centuries. Averroes also provided a description of sunspots in the 12th century. [167] The invention of the telescope in the early 17th century permitted detailed observations of sunspots by Thomas Harriot, Galileo Galilei and other astronomers. Galileo posited that sunspots were on the surface of the Sun rather than small objects passing between Earth and the Sun. [168]

Arabic astronomical contributions include Al-Battani's discovery that the direction of the Sun's apogee (the place in the Sun's orbit against the fixed stars where it seems to be moving slowest) is changing. [169] (In modern heliocentric terms, this is caused by a gradual motion of the aphelion of the Earth's orbit). Ibn Yunus observed more than 10,000 entries for the Sun's position for many years using a large astrolabe. [170]

From an observation of a transit of Venus in 1032, the Persian astronomer and polymath Ibn Sina concluded that Venus is closer to Earth than the Sun. [171] In 1672 Giovanni Cassini and Jean Richer determined the distance to Mars and were thereby able to calculate the distance to the Sun.

In 1666, Isaac Newton observed the Sun's light using a prism, and showed that it is made up of light of many colors. [172] In 1800, William Herschel discovered infrared radiation beyond the red part of the solar spectrum. [173] The 19th century saw advancement in spectroscopic studies of the Sun; Joseph von Fraunhofer recorded more than 600 absorption lines in the spectrum, the strongest of which are still often referred to as Fraunhofer lines. The 20th century brought about several specialized systems for observing the sun, especially at different narrowband wavelengths, such as those using Calcium H (396.9 nm), K (393.37 nm) and Hydrogen-alpha (656.46 nm) filtering.

In the early years of the modern scientific era, the source of the Sun's energy was a significant puzzle. Lord Kelvin suggested that the Sun is a gradually cooling liquid body that is radiating an internal store of heat. [174] Kelvin and Hermann von Helmholtz then proposed a gravitational contraction mechanism to explain the energy output, but the resulting age estimate was only 20 million years, well short of the time span of at least 300 million years suggested by some geological discoveries of that time. [174] [175] In 1890 Joseph Lockyer, who discovered helium in the solar spectrum, proposed a meteoritic hypothesis for the formation and evolution of the Sun. [176]

Not until 1904 was a documented solution offered. Ernest Rutherford suggested that the Sun's output could be maintained by an internal source of heat, and suggested radioactive decay as the source. [177] However, it would be Albert Einstein who would provide the essential clue to the source of the Sun's energy output with his mass–energy equivalence relation E = mc2. [178] In 1920, Sir Arthur Eddington proposed that the pressures and temperatures at the core of the Sun could produce a nuclear fusion reaction that merged hydrogen (protons) into helium nuclei, resulting in a production of energy from the net change in mass. [179] The preponderance of hydrogen in the Sun was confirmed in 1925 by Cecilia Payne using the ionization theory developed by Meghnad Saha. The theoretical concept of fusion was developed in the 1930s by the astrophysicists Subrahmanyan Chandrasekhar and Hans Bethe. Hans Bethe calculated the details of the two main energy-producing nuclear reactions that power the Sun. [180] [181] In 1957, Margaret Burbidge, Geoffrey Burbidge, William Fowler and Fred Hoyle showed that most of the elements in the universe have been synthesized by nuclear reactions inside stars, some like the Sun. [182]

### Solar space missions

The first satellites designed for long term observation of the Sun from interplanetary space were NASA's Pioneers 6, 7, 8 and 9, which were launched between 1959 and 1968. These probes orbited the Sun at a distance similar to that of Earth, and made the first detailed measurements of the solar wind and the solar magnetic field. Pioneer 9 operated for a particularly long time, transmitting data until May 1983. [183] [184]

In the 1970s, two Helios spacecraft and the Skylab Apollo Telescope Mount provided scientists with significant new data on solar wind and the solar corona. The Helios 1 and 2 probes were U.S.–German collaborations that studied the solar wind from an orbit carrying the spacecraft inside Mercury's orbit at perihelion. [185] The Skylab space station, launched by NASA in 1973, included a solar observatory module called the Apollo Telescope Mount that was operated by astronauts resident on the station. [79] Skylab made the first time-resolved observations of the solar transition region and of ultraviolet emissions from the solar corona. [79] Discoveries included the first observations of coronal mass ejections, then called "coronal transients", and of coronal holes, now known to be intimately associated with the solar wind. [185]

In the 1970s, much research focused on the abundances of iron-group elements in the Sun. [186] [187] Although significant research was done, until 1978 it was difficult to determine the abundances of some iron-group elements (e.g. cobalt and manganese) via spectrography because of their hyperfine structures. [186] The first largely complete set of oscillator strengths of singly ionized iron-group elements were made available in the 1960s, [188] and these were subsequently improved. [189] In 1978, the abundances of singly ionized elements of the iron group were derived. [186] Various authors have considered the existence of a gradient in the isotopic compositions of solar and planetary noble gases, [190] e.g. correlations between isotopic compositions of neon and xenon in the Sun and on the planets. [191] Prior to 1983, it was thought that the whole Sun has the same composition as the solar atmosphere. [192] In 1983, it was claimed that it was fractionation in the Sun itself that caused the isotopic-composition relationship between the planetary and solar-wind-implanted noble gases. [192]

In 1980, the Solar Maximum Mission probes was launched by NASA. This spacecraft was designed to observe gamma rays, X-rays and UV radiation from solar flares during a time of high solar activity and solar luminosity. Just a few months after launch, however, an electronics failure caused the probe to go into standby mode, and it spent the next three years in this inactive state. In 1984 Space Shuttle Challenger mission STS-41C retrieved the satellite and repaired its electronics before re-releasing it into orbit. The Solar Maximum Mission subsequently acquired thousands of images of the solar corona before re-entering Earth's atmosphere in June 1989. [193]

Launched in 1991, Japan's Yohkoh (Sunbeam) satellite observed solar flares at X-ray wavelengths. Mission data allowed scientists to identify several different types of flares and demonstrated that the corona away from regions of peak activity was much more dynamic and active than had previously been supposed. Yohkoh observed an entire solar cycle but went into standby mode when an annular eclipse in 2001 caused it to lose its lock on the Sun. It was destroyed by atmospheric re-entry in 2005. [194]

One of the most important solar missions to date has been the Solar and Heliospheric Observatory, jointly built by the European Space Agency and NASA and launched on 2 December 1995. [79] Originally intended to serve a two-year mission, a mission extension through 2012 was approved in October 2009. [195] It has proven so useful that a follow-on mission, the Solar Dynamics Observatory, was launched in February 2010. [196] Situated at the Lagrangian point between Earth and the Sun (at which the gravitational pull from both is equal), SOHO has provided a constant view of the Sun at many wavelengths since its launch. [79] Besides its direct solar observation, SOHO has enabled the discovery of a large number of comets, mostly tiny sungrazing comets that incinerate as they pass the Sun. [197]

All these satellites have observed the Sun from the plane of the ecliptic, and so have only observed its equatorial regions in detail. The Ulysses probe was launched in 1990 to study the Sun's polar regions. It first traveled to Jupiter, to "slingshot" into an orbit that would take it far above the plane of the ecliptic. Once Ulysses was in its scheduled orbit, it began observing the solar wind and magnetic field strength at high solar latitudes, finding that the solar wind from high latitudes was moving at about 750 km/s, which was slower than expected, and that there were large magnetic waves emerging from high latitudes that scattered galactic cosmic rays. [198]

Elemental abundances in the photosphere are well known from spectroscopic studies, but the composition of the interior of the Sun is more poorly understood. A solar wind sample return mission, Genesis , was designed to allow astronomers to directly measure the composition of solar material. [199]

### Unsolved problems

#### Coronal heating

The temperature of the photosphere is approximately 6,000 K, whereas the temperature of the corona reaches 1,000,000–2,000,000 K. [78] The high temperature of the corona shows that it is heated by something other than direct heat conduction from the photosphere. [80]

It is thought that the energy necessary to heat the corona is provided by turbulent motion in the convection zone below the photosphere, and two main mechanisms have been proposed to explain coronal heating. [78] The first is wave heating, in which sound, gravitational or magnetohydrodynamic waves are produced by turbulence in the convection zone. [78] These waves travel upward and dissipate in the corona, depositing their energy in the ambient matter in the form of heat. [206] The other is magnetic heating, in which magnetic energy is continuously built up by photospheric motion and released through magnetic reconnection in the form of large solar flares and myriad similar but smaller events—nanoflares. [207]

Currently, it is unclear whether waves are an efficient heating mechanism. All waves except Alfvén waves have been found to dissipate or refract before reaching the corona. [208] In addition, Alfvén waves do not easily dissipate in the corona. Current research focus has therefore shifted towards flare heating mechanisms. [78]

#### Faint young Sun

Theoretical models of the Sun's development suggest that 3.8 to 2.5 billion years ago, during the Archean eon, the Sun was only about 75% as bright as it is today. Such a weak star would not have been able to sustain liquid water on Earth's surface, and thus life should not have been able to develop. However, the geological record demonstrates that Earth has remained at a fairly constant temperature throughout its history and that the young Earth was somewhat warmer than it is today. One theory among scientists is that the atmosphere of the young Earth contained much larger quantities of greenhouse gases (such as carbon dioxide, methane) than are present today, which trapped enough heat to compensate for the smaller amount of solar energy reaching it. [209]

However, examination of Archaean sediments appears inconsistent with the hypothesis of high greenhouse concentrations. Instead, the moderate temperature range may be explained by a lower surface albedo brought about by less continental area and the lack of biologically induced cloud condensation nuclei. This would have led to increased absorption of solar energy, thereby compensating for the lower solar output. [210]

## Observation by eyes

The brightness of the Sun can cause pain from looking at it with the naked eye; however, doing so for brief periods is not hazardous for normal non-dilated eyes. [211] [212] Looking directly at the Sun (sungazing) causes phosphene visual artifacts and temporary partial blindness. It also delivers about 4 milliwatts of sunlight to the retina, slightly heating it and potentially causing damage in eyes that cannot respond properly to the brightness. [213] [214] Long-duration viewing of the direct Sun with the naked eye can begin to cause UV-induced, sunburn-like lesions on the retina after about 100 seconds, particularly under conditions where the UV light from the Sun is intense and well focused. [215] [216]

Viewing the Sun through light-concentrating optics such as binoculars may result in permanent damage to the retina without an appropriate filter that blocks UV and substantially dims the sunlight. When using an attenuating filter to view the Sun, the viewer is cautioned to use a filter specifically designed for that use. Some improvised filters that pass UV or IR rays, can actually harm the eye at high brightness levels. [217] Brief glances at the midday Sun through an unfiltered telescope can cause permanent damage. [218]

During sunrise and sunset, sunlight is attenuated because of Rayleigh scattering and Mie scattering from a particularly long passage through Earth's atmosphere, [219] and the Sun is sometimes faint enough to be viewed comfortably with the naked eye or safely with optics (provided there is no risk of bright sunlight suddenly appearing through a break between clouds). Hazy conditions, atmospheric dust, and high humidity contribute to this atmospheric attenuation. [220]

An optical phenomenon, known as a green flash, can sometimes be seen shortly after sunset or before sunrise. The flash is caused by light from the Sun just below the horizon being bent (usually through a temperature inversion) towards the observer. Light of shorter wavelengths (violet, blue, green) is bent more than that of longer wavelengths (yellow, orange, red) but the violet and blue light is scattered more, leaving light that is perceived as green. [221]

## Religious aspects

Solar deities play a major role in many world religions and mythologies. [222] Worship of the Sun was central to civilizations such as the ancient Egyptians, the Inca of South America and the Aztecs of what is now Mexico. In religions such as Hinduism, the Sun is still considered a god, he is known as Surya Dev. Many ancient monuments were constructed with solar phenomena in mind; for example, stone megaliths accurately mark the summer or winter solstice (some of the most prominent megaliths are located in Nabta Playa, Egypt; Mnajdra, Malta and at Stonehenge, England); Newgrange, a prehistoric human-built mount in Ireland, was designed to detect the winter solstice; the pyramid of El Castillo at Chichén Itzá in Mexico is designed to cast shadows in the shape of serpents climbing the pyramid at the vernal and autumnal equinoxes.

The ancient Sumerians believed that the Sun was Utu, [223] [224] the god of justice and twin brother of Inanna, the Queen of Heaven, [223] who was identified as the planet Venus. [224] Later, Utu was identified with the East Semitic god Shamash. [223] [224] Utu was regarded as a helper-deity, who aided those in distress, [223] and, in iconography, he is usually portrayed with a long beard and clutching a saw, [223] which represented his role as the dispenser of justice. [223]

From at least the Fourth Dynasty of Ancient Egypt, the Sun was worshipped as the god Ra, portrayed as a falcon-headed divinity surmounted by the solar disk, and surrounded by a serpent. In the New Empire period, the Sun became identified with the dung beetle, whose spherical ball of dung was identified with the Sun. In the form of the sun disc Aten, the Sun had a brief resurgence during the Amarna Period when it again became the preeminent, if not only, divinity for the Pharaoh Akhenaton. [225] [226]

The Egyptians portrayed the god Ra as being carried across the sky in a solar barque, accompanied by lesser gods, and to the Greeks, he was Helios, carried by a chariot drawn by fiery horses. From the reign of Elagabalus in the late Roman Empire the Sun's birthday was a holiday celebrated as Sol Invictus (literally "Unconquered Sun") soon after the winter solstice, which may have been an antecedent to Christmas. Regarding the fixed stars, the Sun appears from Earth to revolve once a year along the ecliptic through the zodiac, and so Greek astronomers categorized it as one of the seven planets (Greek planetes, "wanderer"); the naming of the days of the weeks after the seven planets dates to the Roman era. [227] [228] [229]

In Proto-Indo-European religion, the Sun was personified as the goddess *Seh2ul. [230] [231] Derivatives of this goddess in Indo-European languages include the Old Norse Sól , Sanskrit Surya , Gaulish Sulis , Lithuanian Saulė , and Slavic Solntse. [231] In ancient Greek religion, the sun deity was the male god Helios, [232] who in later times was syncretized with Apollo. [233]

In the Bible, Malachi 4:2 mentions the "Sun of Righteousness" (sometimes translated as the "Sun of Justice"), [234] which some Christians have interpreted as a reference to the Messiah (Christ). [235] In ancient Roman culture, Sunday was the day of the sun god. It was adopted as the Sabbath day by Christians who did not have a Jewish background. The symbol of light was a pagan device adopted by Christians, and perhaps the most important one that did not come from Jewish traditions. In paganism, the Sun was a source of life, giving warmth and illumination to mankind. It was the center of a popular cult among Romans, who would stand at dawn to catch the first rays of sunshine as they prayed. The celebration of the winter solstice (which influenced Christmas) was part of the Roman cult of the unconquered Sun (Sol Invictus). Christian churches were built with an orientation so that the congregation faced toward the sunrise in the East. [236]

Tonatiuh, the Aztec god of the sun, was usually depicted holding arrows and a shield [237] and was closely associated with the practice of human sacrifice. [237] The sun goddess Amaterasu is the most important deity in the Shinto religion, [238] [239] and she is believed to be the direct ancestor of all Japanese emperors. [238]

## Notes

1. All numbers in this article are short scale. One billion is 109, or 1,000,000,000.
2. In astronomical sciences, the term heavy elements (or metals) refers to all chemical elements except hydrogen and helium.
3. Hydrothermal vent communities live so deep under the sea that they have no access to sunlight. Bacteria instead use sulfur compounds as an energy source, via chemosynthesis.
4. Counterclockwise is also the direction of revolution around the Sun for objects in the Solar System and is the direction of axial spin for most objects.
5. A 50 kg adult human has a volume of about 0.05 m3, which corresponds to 13.8 watts, at the volumetric power of the solar center. This is 285 kcal/day, about 10% of the actual average caloric intake and output for humans in non-stressful conditions.
6. Earth's atmosphere near sea level has a particle density of about 2×1025 m−3.
7. If ${\displaystyle \psi }$ is the angle between the north pole of the ecliptic and the north galactic pole then:
${\displaystyle \cos \psi =\cos(\beta _{g})\cos(\beta _{e})\cos(\alpha _{g}-\alpha _{e})+\sin(\beta _{g})\sin(\beta _{e})}$
where ${\displaystyle \beta _{g}}$ = 27° 07′ 42.01″ and ${\displaystyle \alpha _{g}}$ = 12h 51m 26.282s are the declination and right ascension of the north galactic pole, [158] whereas ${\displaystyle \beta _{e}}$ = 66° 33′ 38.6″ and ${\displaystyle \alpha _{e}}$ = 18h 0m 00s are those for the north pole of the ecliptic. (Both pairs of coordinates are for J2000 epoch.) The result of the calculation is 60.19°.

## Related Research Articles

A corona is the outermost layer of a star's atmosphere. It consists of plasma.

In astronomy, the main sequence is a continuous and distinctive band of stars that appears on plots of stellar color versus brightness. These color-magnitude plots are known as Hertzsprung–Russell diagrams after their co-developers, Ejnar Hertzsprung and Henry Norris Russell. Stars on this band are known as main-sequence stars or dwarf stars. These are the most numerous true stars in the universe and include the Sun.

A star is an astronomical object comprising a luminous spheroid of plasma held together by its gravity. The nearest star to Earth is the Sun. Many other stars are visible to the naked eye at night, but their immense distances from Earth make them appear as fixed points of light. The most prominent stars have been categorised into constellations and asterisms, and many of the brightest stars have proper names. Astronomers have assembled star catalogues that identify the known stars and provide standardized stellar designations. The observable universe contains an estimated 1022 to 1024 stars. Only about 4,000 of these stars are visible to the naked eye, all within the Milky Way galaxy.

Sunspots are phenomena on the Sun's photosphere that appear as temporary spots that are darker than the surrounding areas. They are regions of reduced surface temperature caused by concentrations of magnetic flux that inhibit convection. Sunspots appear within active regions, usually in pairs of opposite magnetic polarity. Their number varies according to the approximately 11-year solar cycle.

The solar wind is a stream of charged particles released from the upper atmosphere of the Sun, called the corona. This plasma mostly consists of electrons, protons and alpha particles with kinetic energy between 0.5 and 10 keV. The composition of the solar wind plasma also includes a mixture of materials found in the solar plasma: trace amounts of heavy ions and atomic nuclei such as C, N, O, Ne, Mg, Si, S, and Fe. There are also rarer traces of some other nuclei and isotopes such as P, Ti, Cr, 54Fe and 56Fe, and 58Ni, 60Ni, and 62Ni. Superposed with the solar-wind plasma is the interplanetary magnetic field. The solar wind varies in density, temperature and speed over time and over solar latitude and longitude. Its particles can escape the Sun's gravity because of their high energy resulting from the high temperature of the corona, which in turn is a result of the coronal magnetic field. The boundary separating the corona from the solar wind is called the Alfvén surface.

The photosphere is a star's outer shell from which light is radiated.

A solar flare is an intense localized eruption of electromagnetic radiation in the Sun's atmosphere. Flares occur in active regions and are often, but not always, accompanied by coronal mass ejections, solar particle events, and other solar phenomena. The occurrence of solar flares varies with the 11-year solar cycle.

A chromosphere is the second layer of a star's atmosphere, located above the photosphere and below the solar transition region and corona. The term usually refers to the Sun's chromosphere, but not exclusively.

Wolf 359 is a red dwarf star located in the constellation Leo, near the ecliptic. At a distance of approximately 7.9 light years from Earth, it has an apparent magnitude of 13.54 and can only be seen with a large telescope. Wolf 359 is one of the nearest stars to the Sun; only the Alpha Centauri system, Barnard's Star, and the brown dwarfs Luhman 16 and WISE 0855−0714 are known to be closer. Its proximity to Earth has led to its mention in several works of fiction.

The solar cycle, also known as the solar magnetic activity cycle, sunspot cycle, or Schwabe cycle, is a nearly periodic 11-year change in the Sun's activity measured in terms of variations in the number of observed sunspots on the Sun's surface. Over the period of a solar cycle, levels of solar radiation and ejection of solar material, the number and size of sunspots, solar flares, and coronal loops all exhibit a synchronized fluctuation from a period of minimum activity to a period of a maximum activity back to a period of minimum activity.

A coronal mass ejection (CME) is a significant release of plasma and accompanying magnetic field from the Sun's corona into the heliosphere. CMEs are often associated with solar flares and other forms of solar activity, but a broadly accepted theoretical understanding of these relationships has not been established.

The stellar atmosphere is the outer region of the volume of a star, lying above the stellar core, radiation zone and convection zone.

In plasma physics, an Alfvén wave, named after Hannes Alfvén, is a type of plasma wave in which ions oscillate in response to a restoring force provided by an effective tension on the magnetic field lines.

The solar dynamo is a physical process that generates the Sun's magnetic field. It is explained with a variant of the dynamo theory. A naturally occurring electric generator in the Sun's interior produces electric currents and a magnetic field, following the laws of Ampère, Faraday and Ohm, as well as the laws of fluid dynamics, which together form the laws of magnetohydrodynamics. The detailed mechanism of the solar dynamo is not known and is the subject of current research.

The core of the Sun is considered to extend from the center to about 0.2 to 0.25 of solar radius. It is the hottest part of the Sun and of the Solar System. It has a density of 150 g/cm3 at the center, and a temperature of 15 million kelvins.

In solar physics, a coronal loop is a well-defined arch-like structure in the Sun's atmosphere made up of relatively dense plasma confined and isolated from the surrounding medium by magnetic flux tubes. Coronal loops begin and end at two footpoints on the photosphere and project into the transition region and lower corona. They typically form and dissipate over periods of seconds to days and may span anywhere from 1 to 1,000 megametres in length.

A stellar magnetic field is a magnetic field generated by the motion of conductive plasma inside a star. This motion is created through convection, which is a form of energy transport involving the physical movement of material. A localized magnetic field exerts a force on the plasma, effectively increasing the pressure without a comparable gain in density. As a result, the magnetized region rises relative to the remainder of the plasma, until it reaches the star's photosphere. This creates starspots on the surface, and the related phenomenon of coronal loops.

A red giant is a luminous giant star of low or intermediate mass in a late phase of stellar evolution. The outer atmosphere is inflated and tenuous, making the radius large and the surface temperature around 5,000 K or lower. The appearance of the red giant is from yellow-white to reddish-orange, including the spectral types K and M, sometimes G, but also class S stars and most carbon stars.

A nanoflare is a very small episodic heating event which happens in the corona, the external atmosphere of the Sun.

Solar phenomena are natural phenomena which occur within the atmosphere of the Sun. These phenomena take many forms, including solar wind, radio wave flux, solar flares, coronal mass ejections, coronal heating and sunspots.

## References

1. . Oxford English Dictionary (Online ed.). Oxford University Press. (Subscription or participating institution membership required.)
2. "Helios". Lexico UK English Dictionary. Oxford University Press. Archived from the original on 27 March 2020.
3. . Oxford English Dictionary (Online ed.). Oxford University Press. (Subscription or participating institution membership required.)
4. Pitjeva, E. V.; Standish, E. M. (2009). "Proposals for the masses of the three largest asteroids, the Moon–Earth mass ratio and the Astronomical Unit". Celestial Mechanics and Dynamical Astronomy . 103 (4): 365–372. Bibcode:2009CeMDA.103..365P. doi:10.1007/s10569-009-9203-8. ISSN   1572-9478. S2CID   121374703. Archived from the original on 9 July 2019. Retrieved 13 July 2019.
5. Williams, D.R. (1 July 2013). "Sun Fact Sheet". NASA Goddard Space Flight Center. Archived from the original on 15 July 2010. Retrieved 12 August 2013.
6. Zombeck, Martin V. (1990). Handbook of Space Astronomy and Astrophysics 2nd edition. Cambridge University Press. Archived from the original on 3 February 2021. Retrieved 13 January 2016.
7. Asplund, M.; Grevesse, N.; Sauval, A.J. (2006). "The new solar abundances – Part I: the observations". Communications in Asteroseismology. 147: 76–79. Bibcode:2006CoAst.147...76A. doi:. S2CID   123824232.
8. "Eclipse 99: Frequently Asked Questions". NASA. Archived from the original on 27 May 2010. Retrieved 24 October 2010.
9. Hinshaw, G.; et al. (2009). "Five-year Wilkinson Microwave Anisotropy Probe observations: data processing, sky maps, and basic results". The Astrophysical Journal Supplement Series . 180 (2): 225–245. arXiv:. Bibcode:2009ApJS..180..225H. doi:10.1088/0067-0049/180/2/225. S2CID   3629998.
10. Mamajek, E.E.; Prsa, A.; Torres, G.; et, al. (2015), "IAU 2015 Resolution B3 on Recommended Nominal Conversion Constants for Selected Solar and Planetary Properties", arXiv: [astro-ph.SR]
11. Emilio, Marcelo; Kuhn, Jeff R.; Bush, Rock I.; Scholl, Isabelle F. (2012), "Measuring the Solar Radius from Space during the 2003 and 2006 Mercury Transits", The Astrophysical Journal, 750 (2): 135, arXiv:, Bibcode:2012ApJ...750..135E, doi:10.1088/0004-637X/750/2/135, S2CID   119255559
12. "Solar System Exploration: Planets: Sun: Facts & Figures". NASA. Archived from the original on 2 January 2008.
13. Ko, M. (1999). Elert, G. (ed.). "Density of the Sun". The Physics Factbook. Archived from the original on 13 July 2019. Retrieved 14 July 2014.
14. Bonanno, A.; Schlattl, H.; Paternò, L. (2002). "The age of the Sun and the relativistic corrections in the EOS". Astronomy and Astrophysics . 390 (3): 1115–1118. arXiv:. Bibcode:2002A&A...390.1115B. doi:10.1051/0004-6361:20020749. S2CID   119436299.
15. Connelly, JN; Bizzarro, M; Krot, AN; Nordlund, Å; Wielandt, D; Ivanova, MA (2 November 2012). "The Absolute Chronology and Thermal Processing of Solids in the Solar Protoplanetary Disk". Science. 338 (6107): 651–655. Bibcode:2012Sci...338..651C. doi:10.1126/science.1226919. PMID   23118187. S2CID   21965292.
16. "The Sun's Vital Statistics". Stanford Solar Center. Archived from the original on 14 October 2012. Retrieved 29 July 2008. Citing Eddy, J. (1979). A New Sun: The Solar Results From Skylab. NASA. p. 37. NASA SP-402. Archived from the original on 30 July 2021. Retrieved 12 July 2017.
17. Seidelmann, P.K.; et al. (2000). "Report Of The IAU/IAG Working Group On Cartographic Coordinates And Rotational Elements Of The Planets And Satellites: 2000". Archived from the original on 12 May 2020. Retrieved 22 March 2006.
18. "How Round is the Sun?". NASA. 2 October 2008. Archived from the original on 29 March 2019. Retrieved 7 March 2011.
19. "First Ever STEREO Images of the Entire Sun". NASA. 6 February 2011. Archived from the original on 8 March 2011. Retrieved 7 March 2011.
20. Woolfson, M. (2000). "The origin and evolution of the solar system" (PDF). Astronomy & Geophysics . 41 (1): 12. Bibcode:2000A&G....41a..12W. doi:. Archived (PDF) from the original on 11 July 2020. Retrieved 12 April 2020.
21. Basu, S.; Antia, H.M. (2008). "Helioseismology and Solar Abundances". Physics Reports . 457 (5–6): 217–283. arXiv:. Bibcode:2008PhR...457..217B. doi:10.1016/j.physrep.2007.12.002. S2CID   119302796.
22. Connelly, James N.; Bizzarro, Martin; Krot, Alexander N.; Nordlund, Åke; Wielandt, Daniel; Ivanova, Marina A. (2 November 2012). "The Absolute Chronology and Thermal Processing of Solids in the Solar Protoplanetary Disk". Science . 338 (6107): 651–655. Bibcode:2012Sci...338..651C. doi:10.1126/science.1226919. PMID   23118187. S2CID   21965292.
23. Lattis, James M. (1994). Between Copernicus and Galileo: Christoph Clavius and the Collapse of Ptolemaic Cosmology. Chicago: The University of Chicago. pp. 3–4. ISBN   0-226-46929-8.
24. Barnhart, R.K. (1995). The Barnhart Concise Dictionary of Etymology. HarperCollins. p. 776. ISBN   978-0-06-270084-1.
25. Vladimir Orel (2003) A Handbook of Germanic Etymology, Brill
26. Little, William; Fowler, H.W.; Coulson, J. (1955). . Oxford Universal Dictionary on Historical Principles (3rd ed.). ASIN   B000QS3QVQ.
27. . Oxford English Dictionary (Online ed.). Oxford University Press. (Subscription or participating institution membership required.)
28. "Opportunity's View, Sol 959 (Vertical)". NASA. 15 November 2006. Archived from the original on 22 October 2012. Retrieved 1 August 2007.
29. Barnhart, R.K. (1995). The Barnhart Concise Dictionary of Etymology. HarperCollins. p. 778. ISBN   978-0-06-270084-1.
30. Than, K. (2006). "Astronomers Had it Wrong: Most Stars are Single". Space.com. Archived from the original on 21 December 2010. Retrieved 1 August 2007.
31. Lada, C.J. (2006). "Stellar multiplicity and the initial mass function: Most stars are single". Astrophysical Journal Letters . 640 (1): L63–L66. arXiv:. Bibcode:2006ApJ...640L..63L. doi:10.1086/503158. S2CID   8400400.
32. Zeilik, M.A.; Gregory, S.A. (1998). Introductory Astronomy & Astrophysics (4th ed.). Saunders College Publishing. p. 322. ISBN   978-0-03-006228-5.
33. Falk, S.W.; Lattmer, J.M.; Margolis, S.H. (1977). "Are supernovae sources of presolar grains?". Nature . 270 (5639): 700–701. Bibcode:1977Natur.270..700F. doi:10.1038/270700a0. S2CID   4240932.
34. Burton, W.B. (1986). "Stellar parameters". Space Science Reviews . 43 (3–4): 244–250. doi:10.1007/BF00190626. S2CID   189796439.
35. Bessell, M.S.; Castelli, F.; Plez, B. (1998). "Model atmospheres broad-band colors, bolometric corrections and temperature calibrations for O–M stars". Astronomy and Astrophysics . 333: 231–250. Bibcode:1998A&A...333..231B.
36. "Equinoxes, Solstices, Perihelion, and Aphelion, 2000–2020". US Naval Observatory. 31 January 2008. Archived from the original on 13 October 2007. Retrieved 17 July 2009.
37. "Earth at Perihelion and Aphelion: 2001 to 2100". Archived from the original on 9 July 2019. Retrieved 3 June 2021.
38. Cain, Fraser (15 April 2013). "How long does it take sunlight to reach the Earth?". phys.org. Archived from the original on 2 March 2022. Retrieved 2 March 2022.
39. Simon, A. (2001). The Real Science Behind the X-Files : Microbes, meteorites, and mutants. Simon & Schuster. pp. 25–27. ISBN   978-0-684-85618-6. Archived from the original on 17 April 2021. Retrieved 3 November 2020.
40. Beer, J.; McCracken, K.; von Steiger, R. (2012). Cosmogenic Radionuclides: Theory and Applications in the Terrestrial and Space Environments. Springer Science+Business Media. p. 41. ISBN   978-3-642-14651-0.
41. Phillips, K.J.H. (1995). Guide to the Sun. Cambridge University Press. p. 73. ISBN   978-0-521-39788-9.
42. Godier, S.; Rozelot, J.-P. (2000). "The solar oblateness and its relationship with the structure of the tachocline and of the Sun's subsurface" (PDF). Astronomy and Astrophysics . 355: 365–374. Bibcode:2000A&A...355..365G. Archived from the original (PDF) on 10 May 2011. Retrieved 22 February 2006.
43. Jones, G. (16 August 2012). "Sun is the most perfect sphere ever observed in nature". The Guardian . Archived from the original on 3 March 2014. Retrieved 19 August 2013.
44. Schutz, B.F. (2003). Gravity from the ground up. Cambridge University Press. pp. 98–99. ISBN   978-0-521-45506-0.
45. Phillips, K.J.H. (1995). Guide to the Sun. Cambridge University Press. pp. 78–79. ISBN   978-0-521-39788-9.
46. "The Anticlockwise Solar System". www.spaceacademy.net.au. Australian Space Academy. Archived from the original on 7 August 2020. Retrieved 2 July 2020.
47. Lodders, Katharina (10 July 2003). "Solar System Abundances and Condensation Temperatures of the Elements" (PDF). The Astrophysical Journal. 591 (2): 1220–1247. Bibcode:2003ApJ...591.1220L. CiteSeerX  . doi:10.1086/375492. S2CID   42498829. Archived from the original (PDF) on 7 November 2015. Retrieved 1 September 2015.
Lodders, K. (2003). "Abundances and Condensation Temperatures of the Elements" (PDF). Meteoritics & Planetary Science . 38 (suppl): 5272. Bibcode:2003M&PSA..38.5272L. Archived (PDF) from the original on 13 May 2011. Retrieved 3 August 2008.
48. Hansen, C.J.; Kawaler, S.A.; Trimble, V. (2004). Stellar Interiors: Physical Principles, Structure, and Evolution (2nd ed.). Springer. pp. 19–20. ISBN   978-0-387-20089-7.
49. Hansen, C.J.; Kawaler, S.A.; Trimble, V. (2004). Stellar Interiors: Physical Principles, Structure, and Evolution (2nd ed.). Springer. pp. 77–78. ISBN   978-0-387-20089-7.
50. Hansen, C.J.; Kawaler, S.A.; Trimble, V. (2004). Stellar Interiors: Physical Principles, Structure, and Evolution (2nd ed.). Springer. § 9.2.3. ISBN   978-0-387-20089-7.
51. Iben, I Jnr (1965) "Stellar Evolution. II. The Evolution of a 3 M_{sun} Star from the Main Sequence Through Core Helium Burning". (Astrophysical Journal, vol. 142, p. 1447)
52. Aller, L.H. (1968). "The chemical composition of the Sun and the solar system". Proceedings of the Astronomical Society of Australia. 1 (4): 133. Bibcode:1968PASA....1..133A. doi:10.1017/S1323358000011048. S2CID   119759834.
53. García, R.; et al. (2007). "Tracking solar gravity modes: the dynamics of the solar core". Science . 316 (5831): 1591–1593. Bibcode:2007Sci...316.1591G. doi:10.1126/science.1140598. PMID   17478682. S2CID   35285705.
54. Basu, S.; et al. (2009). "Fresh insights on the structure of the solar core". The Astrophysical Journal . 699 (2): 1403–1417. arXiv:. Bibcode:2009ApJ...699.1403B. doi:10.1088/0004-637X/699/2/1403. S2CID   11044272.
55. "NASA/Marshall Solar Physics". Marshall Space Flight Center. 18 January 2007. Archived from the original on 29 March 2019. Retrieved 11 July 2009.
56. Broggini, C. (2003). Physics in Collision, Proceedings of the XXIII International Conference: Nuclear Processes at Solar Energy. XXIII Physics in Collisions Conference. Zeuthen, Germany. p. 21. arXiv:. Bibcode:2003phco.conf...21B. Archived from the original on 21 April 2017. Retrieved 12 August 2013.
57. Goupil, M.J.; Lebreton, Y.; Marques, J.P.; Samadi, R.; Baudin, F. (2011). "Open issues in probing interiors of solar-like oscillating main sequence stars 1. From the Sun to nearly suns". Journal of Physics: Conference Series . 271 (1): 012031. arXiv:. Bibcode:2011JPhCS.271a2031G. doi:10.1088/1742-6596/271/1/012031. S2CID   4776237.
58. The Borexino Collaboration (2020). "Experimental evidence of neutrinos produced in the CNO fusion cycle in the Sun". Nature . 587 (?): 577–582. arXiv:. Bibcode:2020Natur.587..577B. doi:10.1038/s41586-020-2934-0. PMID   33239797. S2CID   227174644 . Retrieved 26 November 2020.
59. Phillips, K.J.H. (1995). Guide to the Sun. Cambridge University Press. pp. 47–53. ISBN   978-0-521-39788-9.
60. Zirker, J.B. (2002). Journey from the Center of the Sun. Princeton University Press. pp.  15–34. ISBN   978-0-691-05781-1.
61. Shu, F.H. (1982). The Physical Universe: An Introduction to Astronomy. University Science Books. p.  102. ISBN   978-0-935702-05-7.
62. "Ask Us: Sun". Cosmicopia. NASA. 2012. Archived from the original on 3 September 2018. Retrieved 13 July 2017.
63. Cohen, H. (9 November 1998). "Table of temperatures, power densities, luminosities by radius in the Sun". Contemporary Physics Education Project. Archived from the original on 29 November 2001. Retrieved 30 August 2011.
64. "Lazy Sun is less energetic than compost". Australian Broadcasting Corporation . 17 April 2012. Archived from the original on 6 March 2014. Retrieved 25 February 2014.
65. Haubold, H.J.; Mathai, A.M. (1994). "Solar Nuclear Energy Generation & The Chlorine Solar Neutrino Experiment". AIP Conference Proceedings . 320 (1994): 102–116. arXiv:. Bibcode:1995AIPC..320..102H. CiteSeerX  . doi:10.1063/1.47009. S2CID   14622069.
66. Myers, S.T. (18 February 1999). "Lecture 11 – Stellar Structure I: Hydrostatic Equilibrium". Introduction to Astrophysics II. Archived from the original on 12 May 2011. Retrieved 15 July 2009.
67. "Sun". World Book at NASA. NASA. Archived from the original on 10 May 2013. Retrieved 10 October 2012.
68. Tobias, S.M. (2005). "The solar tachocline: Formation, stability and its role in the solar dynamo". In A.M. Soward; et al. (eds.). Fluid Dynamics and Dynamos in Astrophysics and Geophysics. CRC Press. pp. 193–235. ISBN   978-0-8493-3355-2. Archived from the original on 29 October 2020. Retrieved 22 August 2020.
69. Mullan, D.J (2000). "Solar Physics: From the Deep Interior to the Hot Corona". In Page, D.; Hirsch, J.G. (eds.). From the Sun to the Great Attractor. Springer. p. 22. ISBN   978-3-540-41064-5. Archived from the original on 17 April 2021. Retrieved 22 August 2020.
70. Abhyankar, K.D. (1977). "A Survey of the Solar Atmospheric Models". Bulletin of the Astronomical Society of India . 5: 40–44. Bibcode:1977BASI....5...40A. Archived from the original on 12 May 2020. Retrieved 12 July 2009.
71. Gibson, Edward G. (1973). The Quiet Sun (NASA SP-303). NASA. ASIN   B0006C7RS0.
72. Shu, F.H. (1991). The Physics of Astrophysics. Vol. 1. University Science Books. ISBN   978-0-935702-64-4.
73. Rast, M.; Nordlund, Å.; Stein, R.; Toomre, J. (1993). "Ionization Effects in Three-Dimensional Solar Granulation Simulations". The Astrophysical Journal Letters . 408 (1): L53–L56. Bibcode:1993ApJ...408L..53R. doi:10.1086/186829.
74. Parnel, C. "Discovery of Helium". University of St Andrews. Archived from the original on 7 November 2015. Retrieved 22 March 2006.
75. Solanki, S.K.; Livingston, W.; Ayres, T. (1994). "New Light on the Heart of Darkness of the Solar Chromosphere". Science . 263 (5143): 64–66. Bibcode:1994Sci...263...64S. doi:10.1126/science.263.5143.64. PMID   17748350. S2CID   27696504.
76. De Pontieu, B.; et al. (2007). "Chromospheric Alfvénic Waves Strong Enough to Power the Solar Wind". Science . 318 (5856): 1574–1577. Bibcode:2007Sci...318.1574D. doi:10.1126/science.1151747. PMID   18063784. S2CID   33655095.
77. Hansteen, V.H.; Leer, E.; Holzer, T.E. (1997). "The role of helium in the outer solar atmosphere". The Astrophysical Journal . 482 (1): 498–509. Bibcode:1997ApJ...482..498H. doi:.
78. Erdèlyi, R.; Ballai, I. (2007). "Heating of the solar and stellar coronae: a review". Astron. Nachr. 328 (8): 726–733. Bibcode:2007AN....328..726E. doi:.
79. Dwivedi, B.N. (2006). "Our ultraviolet Sun" (PDF). Current Science . 91 (5): 587–595. Archived (PDF) from the original on 25 October 2020. Retrieved 22 March 2015.
80. Russell, C.T. (2001). "Solar wind and interplanetary magnetic filed: A tutorial" (PDF). In Song, Paul; Singer, Howard J.; Siscoe, George L. (eds.). Space Weather (Geophysical Monograph). American Geophysical Union. pp. 73–88. ISBN   978-0-87590-984-4. Archived (PDF) from the original on 1 October 2018. Retrieved 11 July 2009.
81. A.G, Emslie; J.A., Miller (2003). "Particle Acceleration". In Dwivedi, B.N. (ed.). Dynamic Sun. Cambridge University Press. p. 275. ISBN   978-0-521-81057-9.
82. "A Star with two North Poles". Science @ NASA. NASA. 22 April 2003. Archived from the original on 18 July 2009.
83. Riley, P.; Linker, J.A.; Mikić, Z. (2002). "Modeling the heliospheric current sheet: Solar cycle variations". Journal of Geophysical Research . 107 (A7): SSH 8–1. Bibcode:2002JGRA..107.1136R. doi:. CiteID 1136.
84. "The Distortion of the Heliosphere: Our Interstellar Magnetic Compass" (Press release). European Space Agency. 2005. Archived from the original on 4 June 2012. Retrieved 22 March 2006.
85. Anderson, Rupert W. (2015). The Cosmic Compendium: Interstellar Travel. pp. 163–164. ISBN   978-1-329-02202-7.
86. "Voyager - the Interstellar Mission". Archived from the original on 14 September 2017. Retrieved 14 May 2021.
87. Dunbar, Brian (2 March 2015). "Components of the Heliosphere". NASA. Archived from the original on 8 August 2021. Retrieved 20 March 2021.
88. Hatfield, Miles (13 December 2021). "NASA Enters the Solar Atmosphere for the First Time". NASA. This article incorporates text from this source, which is in the public domain .
89. "GMS: Animation: NASA's Parker Solar Probe Enters Solar Atmosphere". svs.gsfc.nasa.gov. 14 December 2021. Retrieved 30 July 2022.
90. "SVS: Parker Solar Probe: Crossing the Alfven Surface". svs.gsfc.nasa.gov. 14 December 2021. Retrieved 30 July 2022. This article incorporates text from this source, which is in the public domain .
91. "What Color is the Sun?". Universe Today. Archived from the original on 25 May 2016. Retrieved 23 May 2016.
92. "What Color is the Sun?". Stanford Solar Center. Archived from the original on 30 October 2017. Retrieved 23 May 2016.
93. Wilk, S.R. (2009). "The Yellow Sun Paradox". Optics & Photonics News : 12–13. Archived from the original on 18 June 2012.
94. Karl S. Kruszelnicki (17 April 2012). "Dr Karl's Great Moments In Science: Lazy Sun is less energetic than compost". Australian Broadcasting Corporation . Archived from the original on 6 March 2014. Retrieved 25 February 2014. Every second, the Sun burns 620 million tonnes of hydrogen...
95. "Construction of a Composite Total Solar Irradiance (TSI) Time Series from 1978 to present". Archived from the original on 1 August 2011. Retrieved 5 October 2005.
96. El-Sharkawi, Mohamed A. (2005). Electric energy. CRC Press. pp. 87–88. ISBN   978-0-8493-3078-0.
97. "Solar radiation" (PDF). Archived (PDF) from the original on 1 November 2012. Retrieved 29 December 2012.
98. "Reference Solar Spectral Irradiance: Air Mass 1.5". Archived from the original on 12 May 2019. Retrieved 12 November 2009.
99. Phillips, K.J.H. (1995). Guide to the Sun. Cambridge University Press. pp. 14–15, 34–38. ISBN   978-0-521-39788-9.
100. Barsh, G.S. (2003). "What Controls Variation in Human Skin Color?". PLOS Biology . 1 (1): e7. doi:10.1371/journal.pbio.0000027. PMC  . PMID   14551921.
101. "Ancient sunlight". Technology Through Time. NASA. 2007. Archived from the original on 15 May 2009. Retrieved 24 June 2009.
102. Stix, M. (2003). "On the time scale of energy transport in the sun". Solar Physics . 212 (1): 3–6. Bibcode:2003SoPh..212....3S. doi:10.1023/A:1022952621810. S2CID   118656812.
103. Schlattl, H. (2001). "Three-flavor oscillation solutions for the solar neutrino problem". Physical Review D . 64 (1): 013009. arXiv:. Bibcode:2001PhRvD..64a3009S. doi:10.1103/PhysRevD.64.013009. S2CID   117848623.
104. Charbonneau, P. (2014). "Solar Dynamo Theory". Annual Review of Astronomy and Astrophysics. 52: 251–290. Bibcode:2014ARA&A..52..251C. doi:10.1146/annurev-astro-081913-040012. S2CID   17829477.
105. Zirker, J.B. (2002). Journey from the Center of the Sun. Princeton University Press. pp.  119–120. ISBN   978-0-691-05781-1.
106. Lang, Kenneth R. (2008). The Sun from Space. Springer-Verlag. p. 75. ISBN   978-3-540-76952-1.
107. Wang, Y.-M.; Sheeley, N.R. (2003). "Modeling the Sun's Large-Scale Magnetic Field during the Maunder Minimum". The Astrophysical Journal . 591 (2): 1248–1256. Bibcode:2003ApJ...591.1248W. doi:10.1086/375449. S2CID   7332154.
108. "The Largest Sunspot in Ten Years". Goddard Space Flight Center. 30 March 2001. Archived from the original on 23 August 2007. Retrieved 10 July 2009.
109. Hale, G.E.; Ellerman, F.; Nicholson, S.B.; Joy, A.H. (1919). "The Magnetic Polarity of Sun-Spots". The Astrophysical Journal. 49: 153. Bibcode:1919ApJ....49..153H. doi:10.1086/142452.
110. "NASA Satellites Capture Start of New Solar Cycle". PhysOrg. 4 January 2008. Archived from the original on 6 April 2008. Retrieved 10 July 2009.
111. "Sun flips magnetic field". CNN . 16 February 2001. Archived from the original on 21 January 2015. Retrieved 11 July 2009.
112. Phillips, T. (15 February 2001). "The Sun Does a Flip". NASA. Archived from the original on 12 May 2009. Retrieved 11 July 2009.
113. Zirker, J.B. (2002). Journey from the Center of the Sun. Princeton University Press. pp.  120–127. ISBN   978-0-691-05781-1.
114. Willson, R.C.; Hudson, H.S. (1991). "The Sun's luminosity over a complete solar cycle". Nature . 351 (6321): 42–44. Bibcode:1991Natur.351...42W. doi:10.1038/351042a0. S2CID   4273483.
115. Eddy, John A. (June 1976). "The Maunder Minimum". Science . 192 (4245): 1189–1202. Bibcode:1976Sci...192.1189E. doi:10.1126/science.192.4245.1189. JSTOR   17425839. PMID   17771739. S2CID   33896851.
116. Lean, J.; Skumanich, A.; White, O. (1992). "Estimating the Sun's radiative output during the Maunder Minimum". Geophysical Research Letters . 19 (15): 1591–1594. Bibcode:1992GeoRL..19.1591L. doi:10.1029/92GL01578. Archived from the original on 11 May 2020. Retrieved 16 December 2019.
117. Mackay, R.M.; Khalil, M.A.K (2000). "Greenhouse gases and global warming". In Singh, S.N. (ed.). Trace Gas Emissions and Plants. Springer. pp. 1–28. ISBN   978-0-7923-6545-7. Archived from the original on 17 April 2021. Retrieved 3 November 2020.
118. Johnson-Groh, Mara (17 December 2019). "SDO sees new kind of magnetic explosion on sun". phys.org. Archived from the original on 27 January 2022. Retrieved 28 July 2022.
119. "THE 100 NEAREST STAR SYSTEMS". www.astro.gsu.edu. Archived from the original on 12 November 2007. Retrieved 30 April 2022.
120. Zirker, Jack B. (2002). Journey from the Center of the Sun. Princeton University Press. pp.  7–8. ISBN   978-0-691-05781-1.
121. Amelin, Y.; Krot, A.; Hutcheon, I.; Ulyanov, A. (2002). "Lead isotopic ages of chondrules and calcium-aluminum-rich inclusions". Science . 297 (5587): 1678–1683. Bibcode:2002Sci...297.1678A. doi:10.1126/science.1073950. PMID   12215641. S2CID   24923770.
122. Baker, J.; Bizzarro, M.; Wittig, N.; Connelly, J.; Haack, H. (2005). "Early planetesimal melting from an age of 4.5662 Gyr for differentiated meteorites". Nature . 436 (7054): 1127–1131. Bibcode:2005Natur.436.1127B. doi:10.1038/nature03882. PMID   16121173. S2CID   4304613.
123. Williams, J. (2010). "The astrophysical environment of the solar birthplace". Contemporary Physics. 51 (5): 381–396. arXiv:. Bibcode:2010ConPh..51..381W. CiteSeerX  . doi:10.1080/00107511003764725. S2CID   118354201.
124. Goldsmith, D.; Owen, T. (2001). The search for life in the universe. University Science Books. p. 96. ISBN   978-1-891389-16-0. Archived from the original on 30 October 2020. Retrieved 22 August 2020.
125. Source, News Staff / (12 August 2022). "ESA's Gaia Mission Sheds New Light on Past and Future of Our Sun | Sci.News". Sci.News: Breaking Science News. Retrieved 15 August 2022.
126. Carroll, Bradley W.; Ostlie, Dal A (2017). An introduction to modern astrophysics (Second ed.). Cambridge, United Kingdom. pp. 350, 447, 448, 457. ISBN   9781108422161.
127. "Earth Won't Die as Soon as Thought". 22 January 2014. Archived from the original on 12 November 2020. Retrieved 24 May 2015.
128. Snyder-Beattie, Andrew E.; Bonsall, Michael B. (30 March 2022). "Catastrophe risk can accelerate unlikely evolutionary transitions". Proceedings of the Royal Society B. 289 (1971). doi:10.1098/rspb.2021.2711. PMC  . PMID   35350860.
129. Nola Taylor Redd. "Red Giant Stars: Facts, Definition & the Future of the Sun". space.com. Archived from the original on 9 February 2016. Retrieved 20 February 2016.
130. Schröder, K.-P.; Connon Smith, R. (2008). "Distant future of the Sun and Earth revisited". Monthly Notices of the Royal Astronomical Society. 386 (1): 155–163. arXiv:. Bibcode:2008MNRAS.386..155S. doi:10.1111/j.1365-2966.2008.13022.x. S2CID   10073988.
131. Boothroyd, A.I.; Sackmann, I.‐J. (1999). "The CNO Isotopes: Deep Circulation in Red Giants and First and Second Dredge‐up". The Astrophysical Journal. 510 (1): 232–250. arXiv:. Bibcode:1999ApJ...510..232B. doi:10.1086/306546. S2CID   561413.
132. "The End Of The Sun". Archived from the original on 22 May 2019. Retrieved 24 May 2015.
133. Vassiliadis, E.; Wood, P.R. (1993). "Evolution of low- and intermediate-mass stars to the end of the asymptotic giant branch with mass loss". The Astrophysical Journal. 413: 641. Bibcode:1993ApJ...413..641V. doi:10.1086/173033.
134. Bloecker, T. (1995). "Stellar evolution of low and intermediate-mass stars. I. Mass loss on the AGB and its consequences for stellar evolution". Astronomy and Astrophysics. 297: 727. Bibcode:1995A&A...297..727B.
135. Bloecker, T. (1995). "Stellar evolution of low- and intermediate-mass stars. II. Post-AGB evolution". Astronomy and Astrophysics. 299: 755. Bibcode:1995A&A...299..755B.
136. John Lewis, ed. (2004). Physics and chemistry of the solar system (2 ed.). Elsevier. p. 147.
137. See Figure 5 and reference in Valentina Zharkova; et al. (24 June 2019). "Oscillations of the baseline of solar magnetic field and solar irradiance on a millennial timescale". Scientific Reports. 9 (1): 9197. arXiv:. doi:10.1038/s41598-019-45584-3. PMC  . PMID   31235834.
138. Paul Jose (April 1965). "Sun's Motion and Sunspots" (PDF). The Astronomical Journal . 70: 193–200. Bibcode:1965AJ.....70..193J. doi:10.1086/109714. Archived (PDF) from the original on 22 March 2020. Retrieved 22 March 2020. The value of 24° comes from (360)(15 J  6 S)/(S  J), where S and J are the periods of Saturn and Jupiter respectively.
139. Zharkova, V. V.; Shepherd, S. J.; Zharkov, S. I.; Popova, E. (4 March 2020). "Retraction Note: Oscillations of the baseline of solar magnetic field and solar irradiance on a millennial timescale". Scientific Reports. 10 (1): 4336. Bibcode:2020NatSR..10.4336Z. doi:. PMC  . PMID   32132618.
140. "Our Local Galactic Neighborhood". NASA. 5 June 2013. Archived from the original on 21 November 2013.
141. Linsky, Jeffrey L.; Redfield, Seth; Tilipman, Dennis (20 November 2019). "The Interface between the Outer Heliosphere and the Inner Local ISM: Morphology of the Local Interstellar Cloud, Its Hydrogen Hole, Strömgren Shells, and 60 Fe Accretion*". The Astrophysical Journal. 886 (1): 41. arXiv:. Bibcode:2019ApJ...886...41L. doi:10.3847/1538-4357/ab498a. ISSN   0004-637X. S2CID   203642080. Archived from the original on 24 March 2022. Retrieved 29 March 2022.
142. Zucker, Catherine; Goodman, Alyssa A.; Alves, João; et al. (January 2022). "Star formation near the Sun is driven by expansion of the Local Bubble". Nature. 601 (7893): 334–337. arXiv:. Bibcode:2022Natur.601..334Z. doi:10.1038/s41586-021-04286-5. ISSN   1476-4687. PMID   35022612. S2CID   245906333. Archived from the original on 17 April 2022. Retrieved 1 April 2022.
143. Alves, João; Zucker, Catherine; Goodman, Alyssa A.; Speagle, Joshua S.; Meingast, Stefan; Robitaille, Thomas; Finkbeiner, Douglas P.; Schlafly, Edward F.; Green, Gregory M. (23 January 2020). "A Galactic-scale gas wave in the Solar Neighborhood". Nature. 578 (7794): 237–239. arXiv:. Bibcode:2020Natur.578..237A. doi:10.1038/s41586-019-1874-z. PMID   31910431. S2CID   210086520. Archived from the original on 24 April 2022. Retrieved 24 April 2022.
144. McKee, Christopher F.; Parravano, Antonio; Hollenbach, David J. (November 2015). "Stars, Gas, and Dark Matter in the Solar Neighborhood". The Astrophysical Journal. 814 (1): 24. arXiv:. Bibcode:2015ApJ...814...13M. doi:10.1088/0004-637X/814/1/13. S2CID   54224451. 13.
145. Linsky, Jeffrey L.; Redfield, Seth; Tilipman, Dennis (November 2019). "The Interface between the Outer Heliosphere and the Inner Local ISM: Morphology of the Local Interstellar Cloud, Its Hydrogen Hole, Strömgren Shells, and 60Fe Accretion". The Astrophysical Journal. 886 (1): 19. arXiv:. Bibcode:2019ApJ...886...41L. doi:10.3847/1538-4357/ab498a. S2CID   203642080. 41.
146. Anglada-Escudé, Guillem; Amado, Pedro J.; Barnes, John; et al. (2016). "A terrestrial planet candidate in a temperate orbit around Proxima Centauri". Nature. 536 (7617): 437–440. arXiv:. Bibcode:2016Natur.536..437A. doi:10.1038/nature19106. PMID   27558064. S2CID   4451513. Archived from the original on 3 October 2021. Retrieved 11 September 2021.
147. "The One Hundred Nearest Star Systems". Georgia State University Astronomy Department. Research Consortium on Nearby Stars (RECONS). 17 September 2007. Archived from the original on 12 November 2007. Retrieved 1 May 2022.
148. Luhman, K. L. (2014). "Discovery of a ~250 K Brown Dwarf at 2 pc from the Sun". The Astrophysical Journal. 786 (2): L18. arXiv:. Bibcode:2014ApJ...786L..18L. doi:10.1088/2041-8205/786/2/L18. S2CID   119102654.
149. Karttunen, Hannu; Oja, Heikki; Donner, Karl Johan; Poutanen, Markku; Kröger, Pekka, eds. (2003). Fundamental Astronomy (4th ed.). Berlin: Springer. p. 414. ISBN   978-3-540-00179-9. OCLC   51003837. Archived from the original on 20 April 2022. Retrieved 1 April 2022.
150. van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID   18759600.
151. Teixeira, T. C.; Kjeldsen, H.; Bedding, T. R.; Bouchy, F.; Christensen-Dalsgaard, J.; Cunha, M. S.; et al. (January 2009). "Solar-like oscillations in the G8 V star τ Ceti". Astronomy and Astrophysics. 494 (1): 237–242. arXiv:. Bibcode:2009A&A...494..237T. doi:10.1051/0004-6361:200810746. S2CID   59353134.
152. Alves, João; Zucker, Catherine; Goodman, Alyssa A.; et al. (2020). "A Galactic-scale gas wave in the solar neighborhood". Nature. 578 (7794): 237–239. arXiv:. Bibcode:2020Natur.578..237A. doi:10.1038/s41586-019-1874-z. PMID   31910431. S2CID   210086520.
153. Lang, Kenneth R. (2013). The Life and Death of Stars. Cambridge University Press. p. 264. ISBN   9781107016385. Archived from the original on 20 April 2022. Retrieved 8 April 2022.
154. Drimmel, R.; Spergel, D. N. (2001). "Three Dimensional Structure of the Milky Way Disk". The Astrophysical Journal . 556 (1): 181–202. arXiv:. Bibcode:2001ApJ...556..181D. doi:10.1086/321556. S2CID   15757160.
155. Abuter, R.; Amorim, A.; Bauböck, M.; Berger, J. P.; Bonnet, H.; Brandner, W.; et al. (May 2019). "A geometric distance measurement to the Galactic center black hole with 0.3% uncertainty". Astronomy & Astrophysics. 625: L10. arXiv:. Bibcode:2019A&A...625L..10G. doi:10.1051/0004-6361/201935656. ISSN   0004-6361. S2CID   119190574. Archived from the original on 20 April 2022. Retrieved 1 April 2022.
156. Leong, Stacy (2002). "Period of the Sun's Orbit around the Galaxy (Cosmic Year)". The Physics Factbook. Archived from the original on 7 January 2019. Retrieved 2 April 2007.
157. Greiner, Walter (2004). Classical Mechanics: Point particles and relativity. New York: Springer. p. 323. ISBN   978-0-387-21851-9. OCLC   56727455. Archived from the original on 20 April 2022. Retrieved 29 March 2022.
158. Reid, M. J.; Brunthaler, A. (2004). "The Proper Motion of Sagittarius A*". The Astrophysical Journal . 616 (2): 872–884. arXiv:. Bibcode:2004ApJ...616..872R. doi:10.1086/424960. S2CID   16568545.
159. Mullen, Leslie (18 May 2001). "Galactic Habitable Zones". Astrobiology Magazine. Archived from the original on 7 August 2011. Retrieved 1 June 2020.
160. Gerhard, O. (2011). "Pattern speeds in the Milky Way". Memorie della Societa Astronomica Italiana, Supplementi. 18: 185. arXiv:. Bibcode:2011MSAIS..18..185G.
161. Bailer-Jones, C. A. L. (1 July 2009). "The evidence for and against astronomical impacts on climate change and mass extinctions: a review". International Journal of Astrobiology. 8 (3): 213–219. arXiv:. Bibcode:2009IJAsB...8..213B. doi:10.1017/S147355040999005X. S2CID   2028999. Archived from the original on 1 April 2022. Retrieved 1 April 2022.
162. Racki, Grzegorz (December 2012). "The Alvarez Impact Theory of Mass Extinction; Limits to its Applicability and the "Great Expectations Syndrome"". Acta Palaeontologica Polonica. 57 (4): 681–702. doi:10.4202/app.2011.0058. ISSN   0567-7920. S2CID   54021858. Archived from the original on 1 April 2022. Retrieved 1 April 2022.
163. Mamajek, Eric E.; Barenfeld, Scott A.; Ivanov, Valentin D.; Kniazev, Alexei Y.; Väisänen, Petri; Beletsky, Yuri; Boffin, Henri M. J. (February 2015). "The Closest Known Flyby of a Star to the Solar System". The Astrophysical Journal Letters. 800 (1): 4. arXiv:. Bibcode:2015ApJ...800L..17M. doi:10.1088/2041-8205/800/1/L17. S2CID   40618530. L17.
164. Leverington, David (2003). Babylon to Voyager and beyond: a history of planetary astronomy. Cambridge University Press. pp. 6–7. ISBN   978-0-521-80840-8.
165. Sider, D. (1973). "Anaxagoras on the Size of the Sun". Classical Philology . 68 (2): 128–129. doi:10.1086/365951. JSTOR   269068. S2CID   161940013.
166. Goldstein, B.R. (1967). "The Arabic Version of Ptolemy's Planetary Hypotheses". Transactions of the American Philosophical Society. 57 (4): 9–12. doi:10.2307/1006040. JSTOR   1006040.
167. Ead, Hamed A. Averroes As A Physician. University of Cairo.
168. "Galileo Galilei (1564–1642)". BBC. Archived from the original on 29 September 2018. Retrieved 22 March 2006.
169. A short History of scientific ideas to 1900, C. Singer, Oxford University Press, 1959, p. 151.
170. The Arabian Science, C. Ronan, pp. 201–244 in The Cambridge Illustrated History of the World's Science, Cambridge University Press, 1983; at pp. 213–214.
171. Goldstein, Bernard R. (March 1972). "Theory and Observation in Medieval Astronomy". Isis . 63 (1): 39–47 [44]. Bibcode:1972Isis...63...39G. doi:10.1086/350839. S2CID   120700705.
172. "Sir Isaac Newton (1643–1727)". BBC Teach. BBC. Archived from the original on 10 March 2015. Retrieved 22 March 2006.
173. "Herschel Discovers Infrared Light". Cool Cosmos. Archived from the original on 25 February 2012. Retrieved 22 March 2006.
174. Thomson, W. (1862). "On the Age of the Sun's Heat". Macmillan's Magazine . 5: 388–393. Archived from the original on 25 September 2006. Retrieved 25 August 2006.
175. Stacey, Frank D. (2000). "Kelvin's age of the Earth paradox revisited". Journal of Geophysical Research . 105 (B6): 13155–13158. Bibcode:2000JGR...10513155S. doi:.
176. Lockyer, J.N. (1890). "The meteoritic hypothesis; a statement of the results of a spectroscopic inquiry into the origin of cosmical systems". London and New York. Bibcode:1890mhsr.book.....L.
177. Darden, L. (1998). "The Nature of Scientific Inquiry". Archived from the original on 17 August 2012. Retrieved 25 August 2006.
178. Hawking, S.W. (2001). The Universe in a Nutshell. Bantam Books. ISBN   978-0-553-80202-3.
179. "Studying the stars, testing relativity: Sir Arthur Eddington". Space Science. European Space Agency. 2005. Archived from the original on 20 October 2012. Retrieved 1 August 2007.
180. Bethe, H.; Critchfield, C. (1938). "On the Formation of Deuterons by Proton Combination". Physical Review . 54 (10): 862. Bibcode:1938PhRv...54Q.862B. doi:10.1103/PhysRev.54.862.2.
181. Bethe, H. (1939). "Energy Production in Stars". Physical Review . 55 (1): 434–456. Bibcode:1939PhRv...55..434B. doi:. PMID   17835673. S2CID   36146598.
182. Burbidge, E.M.; Burbidge, G.R.; Fowler, W.A.; Hoyle, F. (1957). "Synthesis of the Elements in Stars" (PDF). Reviews of Modern Physics . 29 (4): 547–650. Bibcode:1957RvMP...29..547B. doi:. Archived (PDF) from the original on 23 July 2018. Retrieved 12 April 2020.
183. Wade, M. (2008). "Pioneer 6-7-8-9-E". Encyclopedia Astronautica. Archived from the original on 22 April 2006. Retrieved 22 March 2006.
184. "Solar System Exploration: Missions: By Target: Our Solar System: Past: Pioneer 9". NASA. Archived from the original on 2 April 2012. Retrieved 30 October 2010. NASA maintained contact with Pioneer 9 until May 1983
185. Burlaga, L.F. (2001). "Magnetic Fields and plasmas in the inner heliosphere: Helios results". Planetary and Space Science. 49 (14–15): 1619–1627. Bibcode:2001P&SS...49.1619B. doi:10.1016/S0032-0633(01)00098-8. Archived from the original on 13 July 2020. Retrieved 25 August 2019.
186. Biemont, E. (1978). "Abundances of singly ionized elements of the iron group in the Sun". Monthly Notices of the Royal Astronomical Society . 184 (4): 683–694. Bibcode:1978MNRAS.184..683B. doi:.
187. Ross and Aller 1976, Withbroe 1976, Hauge and Engvold 1977, cited in Biemont 1978.
188. Corliss and Bozman (1962 cited in Biemont 1978) and Warner (1967 cited in Biemont 1978)
189. Smith (1976 cited in Biemont 1978)
190. Signer and Suess 1963; Manuel 1967; Marti 1969; Kuroda and Manuel 1970; Srinivasan and Manuel 1971, all cited in Manuel and Hwaung 1983
191. Kuroda and Manuel 1970 cited in Manuel and Hwaung 1983:7
192. Manuel, O.K.; Hwaung, G. (1983). "Solar abundances of the elements". Meteoritics . 18 (3): 209–222. Bibcode:1983Metic..18..209M. doi:10.1111/j.1945-5100.1983.tb00822.x.
193. Burkepile, C.J. (1998). "Solar Maximum Mission Overview". Archived from the original on 5 April 2006. Retrieved 22 March 2006.
194. "Result of Re-entry of the Solar X-ray Observatory "Yohkoh" (SOLAR-A) to the Earth's Atmosphere" (Press release). Japan Aerospace Exploration Agency. 2005. Archived from the original on 10 August 2013. Retrieved 22 March 2006.
195. "Mission extensions approved for science missions". ESA Science and Technology. 7 October 2009. Archived from the original on 2 May 2013. Retrieved 16 February 2010.
196. "NASA Successfully Launches a New Eye on the Sun". NASA Press Release Archives. 11 February 2010. Archived from the original on 10 August 2013. Retrieved 16 February 2010.
197. "Sungrazing Comets". LASCO (US Naval Research Laboratory). Archived from the original on 25 May 2015. Retrieved 19 March 2009.
198. JPL/CALTECH (2005). "Ulysses: Primary Mission Results". NASA. Archived from the original on 6 January 2006. Retrieved 22 March 2006.
199. Calaway, M.J.; Stansbery, Eileen K.; Keller, Lindsay P. (2009). "Genesis capturing the Sun: Solar wind irradiation at Lagrange 1". Nuclear Instruments and Methods in Physics Research B . 267 (7): 1101–1108. Bibcode:2009NIMPB.267.1101C. doi:10.1016/j.nimb.2009.01.132. Archived from the original on 11 May 2020. Retrieved 13 July 2019.
200. "STEREO Spacecraft & Instruments". NASA Missions. 8 March 2006. Archived from the original on 23 May 2013. Retrieved 30 May 2006.
201. Howard, R.A.; Moses, J.D.; Socker, D.G.; Dere, K.P.; Cook, J.W. (2002). "Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI)" (PDF). Advances in Space Research. 29 (12): 2017–2026. Bibcode:2008SSRv..136...67H. doi:. S2CID   122255862. Archived (PDF) from the original on 14 December 2019. Retrieved 25 August 2019.
202. Meghan Bartels. "Our sun will never look the same again thanks to two solar probes and one giant telescope". Space.com. Archived from the original on 2 March 2020. Retrieved 9 March 2020.
203. "Solar Orbiter". www.esa.int. Archived from the original on 29 March 2022. Retrieved 29 March 2022.
204. Kumar, Chethan (2 February 2022). "2 key Gaganyaan crew abort tests, Aditya top priority". The Times of India. Archived from the original on 18 February 2022. Retrieved 2 February 2022.
205. "Aditya L-1: After Chandrayaan 2, ISRO to pursue India's first mission to the Sun in 2020- Technology News, Firstpost". Tech2. 25 July 2019. Archived from the original on 2 August 2019. Retrieved 2 August 2019.
206. Alfvén, H. (1947). "Magneto-hydrodynamic waves, and the heating of the solar corona". Monthly Notices of the Royal Astronomical Society . 107 (2): 211–219. Bibcode:1947MNRAS.107..211A. doi:.
207. Parker, E.N. (1988). "Nanoflares and the solar X-ray corona". Astrophysical Journal . 330 (1): 474. Bibcode:1988ApJ...330..474P. doi:10.1086/166485.
208. Sturrock, P.A.; Uchida, Y. (1981). "Coronal heating by stochastic magnetic pumping". Astrophysical Journal . 246 (1): 331. Bibcode:1981ApJ...246..331S. doi:10.1086/158926. hdl:.
209. Kasting, J.F.; Ackerman, T.P. (1986). "Climatic Consequences of Very High Carbon Dioxide Levels in the Earth's Early Atmosphere". Science . 234 (4782): 1383–1385. Bibcode:1986Sci...234.1383K. doi:10.1126/science.11539665. PMID   11539665. Archived from the original on 26 September 2019. Retrieved 13 July 2019.
210. Rosing, Minik T.; Bird, Dennis K.; Sleep, Norman H.; Bjerrum, Christian J. (1 April 2010). "No climate paradox under the faint early Sun". Nature. 464 (7289): 744–747. Bibcode:2010Natur.464..744R. doi:10.1038/nature08955. PMID   20360739. S2CID   205220182.
211. White, T.J.; Mainster, M.A.; Wilson, P.W.; Tips, J.H. (1971). "Chorioretinal temperature increases from solar observation". Bulletin of Mathematical Biophysics . 33 (1): 1–17. doi: