Energetic neutral atom

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ENA images of the fluctuation of Earth's ring current during a geomagnetic storm that occurred during July 15-16, 2000. The images were generated by the High Energy Neutral Atom (HENA) instrument present on the IMAGE spacecraft. HENA Earth's Ring Current July 2000 Geomagnetic Storm.gif
ENA images of the fluctuation of Earth's ring current during a geomagnetic storm that occurred during July 15–16, 2000. The images were generated by the High Energy Neutral Atom (HENA) instrument present on the IMAGE spacecraft.

Energetic Neutral Atom (ENA) imaging is a technology used to create global images of otherwise invisible phenomena in the magnetospheres of planets and throughout the heliosphere. [1]

Contents

Charged particles— protons, electrons, and various nuclei— emitted from solar wind are the basis of the interstellar medium. These charged particles have the ability to be redirected by magnetic fields such as the magnetic field surrounding the Earth. Occasionally charged particles within the plasma of the solar wind will collide with neutral atoms. This collision results in the previously charged particle becoming a neutrally charged atom. Due to the loss of charge, the atom no longer experiences magnetic attraction while maintaining its gravitational attraction and velocity. These atoms are Energetic Neutral Atoms and the detection of these atoms can be reconstructed to build ENA images. [2]

Earth's magnetosphere preserves its atmosphere and protects life on Earth from cell-damaging radiation. This region of "space weather" is the site of geomagnetic storms that disrupt communications systems and pose radiation hazards to humans traveling in airplanes (at high altitude and latitude) or in orbiting spacecraft. Geomagnetic weather systems have been late to benefit from the satellite imagery taken for granted in weather forecasting and space physics because their origins in magnetospheric plasma frequency present the added problem of invisibility. [1]

The heliosphere shields the Solar System from the majority of cosmic rays, but is so remote that only an imaging technique such as ENA imaging will reveal its properties. The heliosphere's structure is due to the interaction between the solar wind and cold gas from the local interstellar medium. [2]

The creation of ENAs by space plasma was predicted, but their discovery was both deliberate and serendipitous. While some early efforts were made at detection, their signatures also explained inconsistent findings by ion detectors in regions of expected low-ion populations. Ion detectors were co-opted for further ENA detection experiments in other low-ion regions. [2] However, the development of dedicated ENA detectors entailed overcoming significant obstacles in both skepticism and technology. [1] [3]

Although ENAs were observed in space from the 1960s through the 1980s, [2] the first dedicated ENA camera was not flown until 1995 on the Swedish Astrid-1 satellite, [4] to study Earth's magnetosphere wind.

Today, dedicated ENA instruments have provided detailed magnetospheric images from Venus, Mars, Jupiter, and Saturn. Cassini's ENA images of Saturn revealed a unique magnetosphere with complex interactions that have yet to be fully explained. [1] The IMAGE mission's three dedicated ENA cameras observed Earth's magnetosphere from 2000–2005 [5] while the TWINS Mission, launched in 2008, provides stereo ENA imaging of Earth's magnetosphere using simultaneous imaging from two satellites. [6]

The first ever images of the heliosphere boundary, published in October 2009, were made by the ENA instruments aboard the IBEX and Cassini spacecraft, and challenge existing theories about the heliosphere region. [5] [7]

Creation of ENAs

The most abundant ion in space plasma is the hydrogen ion—a bare proton with no excitable electrons to emit visible photons. The occasional visibility of other plasma ions is not sufficient for imaging purposes. [1] ENAs are created in charge-exchange collisions between hot solar plasma ions and a cold neutral background gas. These charge-exchange processes occur with high frequency in planetary magnetospheres and at the edge of the heliosphere. [8]

Charge exchange

A hot plasma ion 'steals' charge from a cold neutral atom to become an Energetic Neutral Atom (ENA) Gruntman ena 01.jpg
A hot plasma ion 'steals' charge from a cold neutral atom to become an Energetic Neutral Atom (ENA)

In a charge-exchange collision between a high energy plasma ion and a cold neutral atom, the ion 'gives' electrons to the neutral atom, producing a cold ion and an energetic neutral atom (ENA). This chemical reaction can be described as:

I1+ + A2 → A1 + I2+

where I1+ is the plasma ion, A2 is a low energy background neutral atom, A1 is the energetic neutral atom (ENA) and I2+ is the lower energy ion.

Species 1 and 2 in this charge-exchange reaction may be the same, such as in proton–hydrogen charge-exchanges: [2]

The ENA leaves the charge exchange in a straight line with the velocity of the original plasma ion. Gruntman ena 02.jpg
The ENA leaves the charge exchange in a straight line with the velocity of the original plasma ion.

H+ + H → H + H+
Additionally, multiple electrons may be exchanged during the ion / neutral reaction. One example of this is the alpha-helium charge-exchange: [2]
He2+ + He → He + He2+

Due to its charge neutrality, the ENA produced in this reaction is only subject to gravitational forces. This is in contrast to charged particles (ions, protons, or electrons) within plasmas that are also subject to electromagnetic forces. Gravitational influences can generally be ignored in space plasmas, so it is common to assume that the ENA preserves the vector momentum of the original pre-interaction plasma ion. [2]

Some ENAs are lost in further charge-exchange, electron collisions and photoionization and polarization, but a great many travel very long distances in space completely undisturbed. [8]

Although plasma recombination and neutral atom acceleration by the solar gravitation may also contribute to an ENA population under certain conditions, the main exception to this creation scenario is the flux of interstellar gas, where neutral particles from the local interstellar medium penetrate the heliosphere with considerable velocity, which classifies them as ENAs as well. [8]

Solar eruptions

Solar flares and coronal mass ejections (CMEs) are the result of eruptions on the surface of the Sun, which may provide another source of ENAs. The STEREO spacecraft detected neutral hydrogen atoms with energies in the 2–5 MeV range from the flare/CME SOL2006-12-05. [10] [11] These particles were not detected with an instrument designed to see ENAs, but there was sufficient ancillary data to make the observation quite unambiguous.

Accelerating ENAs without ionizing them would be difficult, so the observed ENAs were interpreted to have resulted from charge exchange between solar energetic particles (SEP) emitted from the flare/CME with helium atoms in the solar wind. Charge exchange then occurred between the extremely fast SEP protons and the slower solar wind helium atoms, to create the highly neutral hydrogen atoms and slower helium ions. The resulting ENAs propagated through space without being bound to follow the Parker Spiral, so were observed near the Earth before the helium ions that were created in this reaction. This event, which occurred in 2006, was the first observation of ENAs produced by solar eruptions.

Species of ENAs

Proton–hydrogen charge-exchange collisions are often the most important process in space plasma because hydrogen is the most abundant constituent of both plasmas and background gases. Hydrogen charge-exchange occurs at very high velocities involving little exchange of momentum, so the resulting ENAs travel at high speeds.

In general, only a few species are important for ENA formation, namely hydrogen, helium, oxygen and sulfur:

The corresponding neutral gases corresponding to these regions of space are:

Energies

ENA energies are categorized according to instrumentation, not the ENA source ENA Energies.jpg
ENA energies are categorized according to instrumentation, not the ENA source

ENAs are found everywhere in space [2] and are directly observable at energies from 10eV to more than 1 MeV. [8] Their energies are described more with reference to the instruments used for their detection than to their origins.

No single particle analyzer can cover the entire energy interval from 10 eV to beyond 1 MeV. ENA instruments are roughly divided into those that can detect low, medium and high energies in overlapping groups that can be arbitrary and vary from author to author. The low, medium and high energy ranges from one author is shown in the graph [8] along with the energy ranges for the three instruments aboard the IMAGE satellite:

Atoms are usually considered ENAs if they have kinetic energies of gases clearly higher than that can be reached by typical thermodynamic planetary atmospheres, which is usually in excess of 1 eV. This classification is somewhat arbitrary, being driven by the lower limits of ENA measurement instrumentation. The high end limitations are imposed by both measurement techniques and for scientific reasons. [8]

Magnetospheric ENA imaging

Magnetospheres are formed by the solar wind plasma flow around planets with an intrinsic magnetic field (Mercury, Earth, Jupiter, Saturn, Uranus, and Neptune), although planets and moons lacking magnetic fields may sometimes form magnetosphere-like plasma structures. [2] The ionospheres of weakly magnetized planets such as Venus and Mars set up currents that partially deflect the solar wind flow around the planet. [1] ENAs have been observed in a range of planetary magnetospheres throughout the Solar System.

Although magnetospheric plasma fluctuation has very low densities; e.g. near Jupiter's moon Europa, plasma pressures are about 10−13 bar, compared to 1 bar at Earth's surface, [13] and are responsible for magnetospheric dynamics and emissions. For example, geomagnetic storms create serious disturbances in Earth's cable communications systems, navigational systems and power distribution systems.

The strength and orientation of the magnetic field with respect to solar wind flow determines the shape of the magnetosphere. It is usually compressed on the day side and elongated at the night side. [8]

Earth's magnetosphere

The Earth's magnetic field forms a magnetic cavity within the solar wind. Energetic particles in this region of space can have major space weather impacts, including damaging satellites that orbit the Earth and presenting hazards for astronauts. ENA imaging is important to understand the dynamics of these energetic particles, which then allows for mitigation of these space weather effects.

ISEE 1 data validated concept of ENA magnetospheric mapping in 1982 ISEE-1.jpg
ISEE 1 data validated concept of ENA magnetospheric mapping in 1982

ENA detection in Earth's magnetosphere

The first dedicated ENA instrument was launched on a Nike–Tomahawk sounding rocket from Fort Churchill, Manitoba, Canada. This experiment was followed by the launch of a similar instrument on a Javelin sounding rocket in 1970 to an altitude of 840 kilometres (520 mi) at Wallops Island off the coast of Virginia. In 1972 and 1973, the presence of ENA signatures explained inconsistencies in measurements by the IMP-7 and 8 satellites. [2]

ENA data from the NASA/ESA ISEE 1 satellite enabled the construction of the first global image of the storm time ring current in 1982. This was a breakthrough that paved the way for the use of ENAs as a powerful imaging technique. ENAs were also detected during the 1982 magnetic storm by SEEP instrument on the NASA S81-1 spacecraft. In 1989, the exospheric hydrogen atom population around Earth was extensively studied by the NASA Dynamic Explorer (DE-1) satellite. [2]

Launched in 2008, NASA TWINS currently uses ENA detectors on twin satellites to produce 3-D images of Earth's Magnetosphere TWINS-FirstLight-v3 800.jpg
Launched in 2008, NASA TWINS currently uses ENA detectors on twin satellites to produce 3-D images of Earth's Magnetosphere

An instrument with a dedicated high-energy ENA detection channel was flown aboard the 1991 NASA CRRES satellite. A more sophisticated high energy particle instrument was launched on the 1992 NASA/ISAS GEOTAIL spacecraft dedicated to observing Earth's magnetosphere astronomy. Precipitating ENAs can be studied from a low Earth orbit and were measured "looking out" by CRRES and the 1995 Swedish ASTRID satellites. [2]

The new millennium saw ENA Imaging coming into its own. Extensive and detailed observations of the Earth's magnetosphere were made with three ENA instruments aboard the NASA IMAGE Mission from 2000 – 2005. [5] In July 2000, a set of ENA images of the Earth's ring current were made during a geomagnetic storm. (See image at the top of the page.) The storm was triggered by a fast coronal mass ejection that erupted from the Sun on July 14, 2000 and arrived at Earth the next day.

Launched in 2008, the NASA TWINS Mission (two wide-angle Imaging Neutral-atom Spectrometers) provides the capability for stereoscopically imaging the magnetosphere. By imaging ENAs over a broad energy range (~1–100 KeV) using identical instruments on two widely spaced high-altitude, high-inclination spacecraft, TWINS enables 3-dimensional visualization and the resolution of large-scale structures and dynamics within the magnetosphere. [6]

Planetary and other magnetospheres

Magnetospheres of other planets have been studied by flyby spacecraft by orbiters, landers and by Earth-based observations. [2]

Earth's Moon

In February 2009, the ESA SARA LENA instrument aboard India's Chandrayaan-1 detected hydrogen ENAs sputtered from the lunar surface by solar wind protons. Predictions had been that all impacting protons would be absorbed by the lunar regolith but, for an as yet unknown reason, 20% of them are bounced back as low energy hydrogen ENAs. It is hypothesized that the absorbed protons may produce water and hydroxyls in interactions with the regolith. [14] [15] The Moon has no magnetosphere.

Mercury

Launched in 2018, the ESA BepiColombo mission includes ENA instruments to further its objective to study the origin, structure and dynamics of Mercury's magnetic field. [16] [17] The LENA instrument will resemble the SARA instrument sent to Earth's Moon. In addition to magnetospheric ENAs, sputtering from Mercury's surface is also expected.

Venus

Launched in 2005, the ESA VEX (Venus Express) mission's ASPERA (Energetic Neutral Atoms Analyser) consists of two dedicated ENA detectors. [1] In 2006 ENA images were obtained of the interaction between the solar wind and the Venusian upper atmosphere, showing massive escape of planetary oxygen ions. [18]

Mars

Launched in 2003, the ESA MEX (Mars Express) mission's ASPERA instrument has obtained images of the solar wind interacting with the upper Martian atmosphere. [1] The 2004 observations show solar wind plasma and accelerated ions very deep in the ionosphere, down to 270 kilometres (170 mi). above the dayside planetary surface—evidence for solar wind atmospheric erosion. [19]

Jupiter

The GAS [20] instrument on the ESA/NASA Ulysses, launched in 1990, produced unique data on interstellar helium characteristics and ENAs emitted from Jupiter's Io torus. [2] On its Jupiter flyby in 2000, the NASA/ESA/ASI Cassini's INCA instrument confirmed a neutral gas torus associated with Europa. [21] Cassini's ENA images also showed Jupiter's magnetosphere to be dominated by hydrogen atoms ranging from a few to 100 KeV. The atoms are emitted from the planet's atmosphere and from neutral gas tori near the inner Galilean moons. A population of heavier ions was also detected, indicating a significant emission of oxygen and/or sulfur from Jupiter's magnetosphere. [22]

Saturn

The first dedicated ENA camera was flown on the NASA/ESA/ASI Cassini mission, [23] launched in 1997 to study Saturn's magnetosphere. [8] [24]

Saturn's main radiation belt was measured beginning at an altitude of 70,000 kilometres (43,000 mi) from its surface and reaching out to 783,000 kilometres (487,000 mi). Cassini also detected a previously unknown inner belt nearer its surface that is about 6,000 kilometres (3,700 mi) thick. [25]

The dynamics of Saturn's magnetosphere are very different from Earth's. Plasma co-rotates with Saturn in its magnetosphere. Saturn's strong magnetic field and rapid rotation create a strong co-rotational electric field that accelerates plasma in its magnetosphere until it reaches rotation speeds near that of the planet. Because Saturn's moons are essentially 'sitting still' in this very high speed flow, a complex interaction between this plasma and the atmosphere of the moon Titan was observed. [1]

Titan

Cassini's MIMI-INCA ENA instrument has observed Titan on many occasions revealing the structure of the magnetospheric interaction with Titan's dense atmosphere. [26]

Titan, immersed in the fast moving flow of plasma that surrounds Saturn, is shown with intensified ENA on its trailing side. ENAs produced on the leading side travel away from the camera. ENAs Impact Titan Atmpsphere.jpg
Titan, immersed in the fast moving flow of plasma that surrounds Saturn, is shown with intensified ENA on its trailing side. ENAs produced on the leading side travel away from the camera.

Several studies have been performed on Titan's ENA emissions.

Uranus and Neptune

NASA's Voyager 2 took advantage of its orbit to explore Uranus and Neptune, the only spacecraft to ever have done so. In 1986 spacecraft found a Uranian magnetic field that is both large and unusual. [27] More detailed investigations have yet to be carried out.

Heliosphere ENA imaging

The heliosphere is a cavity built up by the solar wind as it presses outward against the pressure of the local interstellar medium (LISM). As the solar wind is a plasma, it is charged and so carries with it the Sun's magnetic field. So the heliosphere can be conceptualised as the Solar System's magnetosphere. The edge of the heliosphere is found far beyond the orbit of Pluto where diminishing solar wind pressure is stopped by the pressure from the LISM. [2]

A possible explanation for the bright ribbon of ENA emission as seen in the IBEX map is that a galactic magnetic field shapes the heliosphere as it drapes over it. The ribbon appears to be produced by the alignment of magnetic fields at th heliosphere. IBEXmagneticfieldinfluence.jpg
A possible explanation for the bright ribbon of ENA emission as seen in the IBEX map is that a galactic magnetic field shapes the heliosphere as it drapes over it. The ribbon appears to be produced by the alignment of magnetic fields at th heliosphere.

The background neutral gas for ENA production at the heliosphere boundary comes predominantly from interstellar gas penetrating the heliosphere. A tiny amount comes from solar wind neutralisation of interplanetary dust near the sun. The heliosphere boundaries are invisible and fluctuating. Although the densities are low, the enormous thickness of the heliosphere makes it a dominant source of ENAs, aside from planetary magnetospheres. [1] Because of the strong dependence of ENA characteristics on heliosphere properties, remote ENA imaging techniques will provide a global view of the structure and dynamics of the heliosphere unattainable by any other means. [2]

The first glimpse of this view was announced in October, 2009, when the NASA IBEX Mission, returned its first image of the unexpected ENA ribbon at the edge of the heliosphere. [28] Results revealed a "very narrow ribbon that is two to three times brighter than anything else in the sky" at the edge of the heliosphere that was not detected by Voyager 1 or Voyager 2 in the region. [28]

Cassini also ENA-imaged the heliosphere and its results complement and extend the IBEX findings, making it possible for scientists to construct the first comprehensive sky map of the heliosphere. Preliminary Cassini data suggest the heliosphere may not have the comet-like shape predicted by existing models but that its shape may be more like a large, round bubble. [7]

Estimates for size of the heliosphere vary between 150 – 200 AU. [a] [1] It is believed that Voyager 1 passed the heliosphere's termination shock in 2002 at approx. 85 – 87 AU [13] while Voyager 2 passed the termination shock in 2007 at about 85 AU. [29] Others place the termination shock at a mean distance of ≈100 AU. [1] Because the solar wind varies by a factor of 2 during the 11 year solar nuclear cycle, there will be variations in the size and shape of the heliosphere, known as heliosphere "breathing." [2]

The huge distances involved creates problems for taking in situ measurements of the various layers of the heliosphere. Voyager 1 and 2 took 27 years and 30 years respectively to arrive at the termination shock. Furthermore, it is worth noting that for large distances to the object, high energy (velocity) and slower ENAs emitted simultaneously would be detected at different times. This time difference varies from 1 - 15 minutes for observing Earth's magnetosphere from a high altitude spacecraft to more than a year for imaging the heliospheric boundary from an Earth orbit. [2]

ENA instruments

Although the study of ENAs promised improvements in the understanding of global magnetospheric and heliosphere processes, its progress was hindered due to initially enormous experimental difficulties.

In the late 1960s, the first direct ENA measurement attempts revealed the difficulties involved. ENA fluxes are very weak, sometimes less than 1 particle per cm2 per second and are typically detected by secondary electron emission upon contact with a solid surface. They exist in regions containing ultraviolet (UV) and extreme ultraviolet (EUV) radiation at fluxes 100 times greater than produce similar emissions. [2]

IMAGE HENA Mission High Energy Neutral Atom camera. Similar to the Cassini INCA instrument. Hena schematic3.gif
IMAGE HENA Mission High Energy Neutral Atom camera. Similar to the Cassini INCA instrument.

An ENA instrument ideally would also specifically:

  1. prevent the entrance of charged particles
  2. suppress background light (photons), particularly UV and EUV radiation
  3. measure mass and energy of incoming ENAs
  4. determine trajectories of incoming ENAs
  5. measure ENA fluxes from 10−3 to 105 per cm2 per steradian per second
  6. measure ENAs ranging in energy from a few eV up to >100 Kev [2]

The challenge to remote sensing via ENAs lies in combining mass spectrometry with the imaging of weak particle fluxes within the stringent limitations imposed by an application on a spacecraft. [8]

Medium and high energy ENA cameras

It became clear very early that to succeed, instruments would have to specialize in specific ENA energies. The following describes, in very simplified terms, a typical instrument function for high (HENA) or medium (MENA) energy instrument, with differences noted. The accompanying illustration is of the HENA camera flown on the NASA IMAGE mission and the description that follows most closely resembles IMAGE mission instruments.

Collimator

A set of electrostatic plates deflect charged particles away from the instrument and collimates the beam of incoming neutral atoms to a few degrees.

Photon rejection and time of flight (TOF)

HENA: TOF is determined by a coincidence detection requirement that turns out to be efficient at eliminating photon background noise as well. An ENA passes through a thin film to a particle energy detector with its energy nearly completely preserved. At the same time, electrons forward scattered from the film are electrostatically ionization deflected to a detector to create a start pulse. The ENA arriving at its solid state detector (SSD) creates the end pulse and its impact position yields its trajectory and therefore path length. The start and stop signals enable TOF to be determined.

If the electrons are scattered by incoming photons, no ENA will be detected to create the stop pulse. If no stop pulse is sensed within an established time appropriate to the energy of the expected particles, the start pulse is discarded. [31]

MENA: Medium energy ENAs would lose too much energy penetrating the film used in the HENA instrument. The thinner film required would be vulnerable to damage by incident UV and EUV. Therefore, photons are prevented from entering the instrument by using a gold diffraction grating. An ultra thin carbon film is mounted on the back of the grating. ENAs pass through the grating and the film to impact a solid state detector (SSD), scattering electrons and allowing path length and TOF determinations as for the HENA above. [32]

Knowing path length and TOF enables velocity to be determined.

Energy

The solid state detector (SSD) impacted by the ENA after it passes through the foil registers its energy. The small energy loss due to passing through the foil is handled by instrument calibration.

Mass

Knowing the energy and velocity, the mass of the particle can be calculated from energy = mv2/2. Alternatively, the number of scattered electrons detected can also serve to measure the mass of the ENA. [1]

Mass resolution requirements are normally modest, requiring at most distinguishing among hydrogen (1 AMU), helium (4 AMU), and oxygen (16 AMU) atoms with sulfur (32 AMU) also expected in Jupiter's magnetosphere. [1] [2]

2D and 3D imaging

Usually, obtaining images from a spinning spacecraft provides the second dimension of direction identification. By combining synchronized observations from two different satellites, stereo imaging becomes possible. [2] Results from the TWINS Mission are eagerly awaited, as two viewing points will provide substantially more information about the 3-D nature of Earth's magnetosphere.

Low energy ENA cameras

While the collimator is similar, low-energy instruments such as the NASA GSFC LENA use a foil-stripping technique. Incident ENAs interact with a surface such as tungsten to generate ions that are then analysed by an ion spectrometer. [1] [33] [34]

Because of the need to detect atoms sputtered from the lunar surface as well lighter ENAs, the ESA LENA on the Chandrayaan-1 incorporated a mass spectrometer designed to resolve heavier masses including sodium, potassium, and iron. [14]

Future

As of 2005, a total of only six dedicated ENA detectors had been flown. [1] The launch of instruments aboard in the TWINS and IBEX missions brings the total to nine in 2009 – a 50% increase in only 4 years. Space plasma observation using ENA imaging is an emerging technology that is finally coming into its own.

Several improvements are still needed to perfect the technique. Although the angular resolution has now decreased to a few degrees and different species can be separated, one challenge is to expand the energy range upwards to about 500 Kev. This high energy range covers most of the plasma pressure of Earth's inner magnetosphere as well as some of the higher-energy radiation belts so is desirable for terrestrial ENA imaging. [1]

For lower energy ENAs, below 1 keV, the imaging techniques are completely different and rely on the spectroscopic analysis of ions stripped from a surface by the impinging ENA. Improvements in sub-keV measurements will be needed to image Mercury's magnetosphere due to the consequences of its smaller magnetic field and its smaller geometry. [1]

Importance for Earth

The heliosphere is a protective cocoon for the Solar System, just as the Earth's magnetosphere is a protective cocoon for the Earth. The insight provided by ENAs into the behaviour of space plasma has been pivotal to the understanding of the space environment.

Without the magnetosphere, Earth would be subject to direct bombardment by the solar wind and may be unable to retain an atmosphere. In addition to increased exposure to solar radiation, life on Earth would likely not be possible without the magnetosphere. Similarly, the heliosphere protects the Solar System from the majority of otherwise damaging cosmic rays, with the remainder being deflected by the Earth's magnetosphere.

Although most orbiting satellites are protected by the magnetosphere, geomagnetic storms induce currents in conductors that disrupt communications both in space and in cables on the ground. Understanding the magnetosphere and the ring current and its interaction with the solar wind during high solar activity allows satellites and other space missions to be better protected.

Astronauts on deep space missions will not have Earth's protections so understanding the factors that may affect their exposure to cosmic rays and the solar wind is critical to crewed space exploration. [35] [36] [37]

Notes

^ Astronomers measure distances within the Solar System in astronomical units (AU). One AU equals the average distance between the centers of Earth and the Sun, or 149,598,000 kilometres (92,956,000 mi). Pluto is about 38 AU from the Sun and Jupiter is about 5.2 AU from the Sun. One light-year is 63,240 AU.

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Heliophysics is the physics of the Sun and its connection with the Solar System. NASA defines heliophysics as "(1) the comprehensive new term for the science of the Sun - Solar System Connection, (2) the exploration, discovery, and understanding of Earth's space environment, and (3) the system science that unites all of the linked phenomena in the region of the cosmos influenced by a star like our Sun."

<span class="mw-page-title-main">Magnetosphere of Jupiter</span> Cavity created in the solar wind

The magnetosphere of Jupiter is the cavity created in the solar wind by Jupiter's magnetic field. Extending up to seven million kilometers in the Sun's direction and almost to the orbit of Saturn in the opposite direction, Jupiter's magnetosphere is the largest and most powerful of any planetary magnetosphere in the Solar System, and by volume the largest known continuous structure in the Solar System after the heliosphere. Wider and flatter than the Earth's magnetosphere, Jupiter's is stronger by an order of magnitude, while its magnetic moment is roughly 18,000 times larger. The existence of Jupiter's magnetic field was first inferred from observations of radio emissions at the end of the 1950s and was directly observed by the Pioneer 10 spacecraft in 1973.

<i>Polar</i> (satellite) NASA science spacecraft which studied the polar magnetosphere until 2008

The Global Geospace Science (GGS) Polar satellite was a NASA science spacecraft designed to study the polar magnetosphere and aurorae. It was launched into orbit in February 1996, and continued operations until the program was terminated in April 2008. The spacecraft remains in orbit, though it is now inactive. Polar is the sister ship to GGS Wind.

<span class="mw-page-title-main">Magnetospheric Multiscale Mission</span> Four NASA robots studying Earths magnetosphere (2015-present)

The Magnetospheric Multiscale (MMS) Mission is a NASA robotic space mission to study the Earth's magnetosphere, using four identical spacecraft flying in a tetrahedral formation. The spacecraft were launched on 13 March 2015 at 02:44 UTC. The mission is designed to gather information about the microphysics of magnetic reconnection, energetic particle acceleration, and turbulence⁠ — processes that occur in many astrophysical plasmas. As of March 2020, the MMS spacecraft have enough fuel to remain operational until 2040.

<span class="mw-page-title-main">TWINS</span> NASA Experiments of the Explorer program

Two Wide-Angle Imaging Neutral-Atom Spectrometers (TWINS) are a pair of NASA instruments aboard two United States National Reconnaissance Office (NRO) satellites in Molniya orbits. TWINS was designed to provide stereo images of the Earth's ring current. The first instrument, TWINS-1, was launched aboard USA-184 on 28 June 2006. TWINS-2 followed aboard USA-200 on 13 March 2008.

<span class="mw-page-title-main">Heliophysics Science Division</span>

The Heliophysics Science Division of the Goddard Space Flight Center (NASA) conducts research on the Sun, its extended Solar System environment, and interactions of Earth, other planets, small bodies, and interstellar gas with the heliosphere. Division research also encompasses geospace—Earth's uppermost atmosphere, the ionosphere, and the magnetosphere—and the changing environmental conditions throughout the coupled heliosphere.

<span class="mw-page-title-main">JEDI</span> Radiometer and particle detector on the Juno spacecraft

JEDI (Jupiter Energetic-particle Detector Instrument) is an instrument on the Juno spacecraft orbiting planet Jupiter. JEDI coordinates with the several other space physics instruments on the Juno spacecraft to characterize and understand the space environment of Jupiter's polar regions, and specifically to understand the generation of Jupiter's powerful aurora. It is part of a suite of instruments to study the magnetosphere of Jupiter. JEDI consists of three identical detectors that use microchannel plates and foil layers to detect the energy, angle, and types of ion within a certain range. It can detect electrons between 40 and 500 keV (Kilo electron-volts), and hydrogen and oxygen from a few tens of keV to less than 1000 keV (1 MeV). JEDI uses radiation-hardened Application Specific Integrated Circuits (ASIC)s. JEDI was turned on in January 2016 while still en route to Jupiter, to study interplanetary space. JEDI uses solid state detectors (SSDs) to measure the total energy (E) of both the ions and the electrons. The MCP anodes and the SSD arrays are configured to determine the directions of arrivals of the incoming charged particles. The instruments also use fast triple coincidence and optimum shielding to suppress penetrating background radiation and incoming UV foreground.

<span class="mw-page-title-main">David J. McComas</span>

David John McComas is an American space physicist, Vice President for Princeton Plasma Physics Laboratory, and Professor of Astrophysical Sciences and leads the Space Physics at Princeton Group at Princeton University. He had been Assistant Vice President for Space Science and Engineering at the Southwest Research Institute, Adjoint Professor of Physics at the University of Texas at San Antonio (UTSA), and was the founding director of the Center for Space Science and Exploration at Los Alamos National Laboratory. He is noted for his extensive accomplishments in experimental space plasma physics, including leading instruments and missions to study the heliosphere and solar wind: IMAP, IBEX, TWINS, Ulysses/SWOOPS, ACE/SWEPAM, and Parker Solar Probe. He received the National Academy of Science's 2023 Arctowski Medal, European Geosciences Union 2022 Hannes Alfven Medal, SCOSTEP 2022 Distinguished Scientist Award, a NASA Exceptional Public Service Medal in 2015, the 2014 COSPAR Space Science Award, and the American Geophysical Union 1993 Macelwane Medal.

<span class="mw-page-title-main">SMILE (spacecraft)</span> Chinese–European satellite studying Earths magnetosphere

Solar wind Magnetosphere Ionosphere Link Explorer (SMILE) is a planned joint venture mission between the European Space Agency and the Chinese Academy of Sciences. SMILE will image for the first time the magnetosphere of the Sun in soft X-rays and UV during up to 40 hours per orbit, improving our understanding of the dynamic interaction between the solar wind and Earth's magnetosphere. The prime science questions of the SMILE mission are

<span class="mw-page-title-main">Interstellar Mapping and Acceleration Probe</span> Planned NASA heliophysics mission

The Interstellar Mapping and Acceleration Probe(IMAP) is a heliophysics mission that will simultaneously investigate two important and coupled science topics in the heliosphere: the acceleration of energetic particles and interaction of the solar wind with the local interstellar medium. These science topics are coupled because particles accelerated in the inner heliosphere play crucial roles in the outer heliospheric interaction. In 2018, NASA selected a team led by David J. McComas of Princeton University to implement the mission, which is currently planned to launch in late April to late May 2025. IMAP will be a Sun-tracking spin-stabilized satellite in orbit about the Sun–Earth L1 Lagrange point with a science payload of ten instruments. IMAP will also continuously broadcast real-time in-situ data that can be used for space weather prediction.

The Solar-Terrestrial Observer for the Response of the Magnetosphere (STORM) was one of five mission proposals selected to proceed to Phase A concept studies as part of the 2019 NASA Heliophysics Medium Class Explorer Announcement of Opportunity. STORM will provide the first-ever global view of the Sun-Earth system. STORM takes simultaneous observations of the solar wind and the response of Earth’s magnetosphere, including the magnetopause, auroral oval, and ring current dynamics, using global multi-spectral and neutral atom imaging to quantify the global circulation of the energy that powers space weather.

References

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