Modern Maximum

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The Modern Maximum, also called the Solar Modern Maximum, refers to a period of intensifying solar activity during one solar cycle. [1] In essence, the Sun undergoes a cycle every 11 years, and during this cycle, the Sun will generally have a large increase in activity, which is why it is known as the Solar Modern Maximum, which produces higher energy outputs, solar eruptions, and a large number of sunspots. [1] Despite the higher energy outputs, the Sun influence isn't responsible for the recent decades warming trend. [2]

Contents

History of sunspot number observations, showing the recent elevated activity Sunspot Numbers.png
History of sunspot number observations, showing the recent elevated activity

Solar cycle

Much information is still unknown; however, researchers have come to a more recent conclusion as to why the Sun may experience these moments of intensity during the Solar Modern Maximum. Recent studies state that during the Modern Maximum event, scientists recorded that the Sun's magnetic poles will begin to flip and eventually reverse completely, and throughout the change in polarity, the Sun will start to experience microbursts of energy due to the changes within its very large magnetic field. [1] The main concern with the changes in polarity is the degree to which it affects the Sun's total solar irradiance, which is a measure of the total energy that is produced from its luminosity. Given that the Earth relies on this energy source in order for life to thrive, major changes could be detrimental. [3] However, recent reports have stated that the changes in solar irradiance experienced in these short cycles are often minimal, equivalent to a change of 0.15% in most cases. This leads scientists to believe that these short periods of time will not greatly affect the overall greenhouse effect, although these short cycles over long periods of time could have measurable impacts. [1]

This maximum period is a natural example of solar variation, and one of many that are known from proxy records of past solar variability. The Modern Maximum reached a double peak once in the 1950s and again during the 1990s. For example, scientists theorized that the Modern Solar Maximum which occurred in 1950-1980 brought a significant cooling phase through parts of the North Atlantic region with Greenland experiencing a major cooling cycle. [4]

Effects on the Earth

The modern solar maximum could be a larger part of Earth's ongoing climate change than once thought. To start, Greenland has an ongoing project known as the Greenland ice core project, which is designed to represent the possible temperature variations that Greenland has experienced over thousands of years. [4] Scientists use argon and nitrogen isotopes trapped within air pockets to collect data on temperature fluctuations during certain periods. [4] Using this method, scientists found a series of data that suggests solar variability within the Sun's modern maximum cycles could have been the main cause of the great cooling that Greenland experienced from 1970 to 1990. [4] After taking a look at previous solar records, it was found that between 1950 and the early 1980s the Sun had experienced very high solar activity during the modern maximum cycle. [4]

This leads many researchers to suggest that higher solar activity could relate to larger cold spells which could be experienced either globally or throughout smaller regions. To test this theory, data needs to be collected that can indicate when the Sun will begin to enter a cycle of high or low solar activity this way temperature fluctuations can be tested and recorded. One-way scientists have recorded different solar cycles is by examining sunspots that are currently on the star and comparing them with earlier known sunspot occurrences. [5] For example, the largest known recorded number of sunspots on the Sun was during the 20th century, and these values have not been seen since the late 18th century. [5] Also, as mentioned earlier Greenland had experienced a very large cold spell at the time of this solar cycle. [4]  

Related Research Articles

<span class="mw-page-title-main">Sun</span> Star at the center of the Solar System

The Sun is the star at the center of the Solar System. It is a massive, hot ball of plasma, inflated and heated by energy produced by nuclear fusion reactions at its core. Part of this energy is emitted from its surface as visible light, ultraviolet, and infrared radiation, providing most of the energy for life on Earth. The Sun has been an object of veneration in many cultures. It has been a central subject for astronomical research since antiquity.

<span class="mw-page-title-main">Sunspot</span> Temporary spots on the Suns surface

Sunspots are temporary spots on the Sun's surface that are darker than the surrounding area. 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.

<span class="mw-page-title-main">Sunlight</span> Light emitted by the Sun

Sunlight is a portion of the electromagnetic radiation given off by the Sun, in particular infrared, visible, and ultraviolet light. On Earth, sunlight is scattered and filtered through Earth's atmosphere as daylight when the Sun is above the horizon. When direct solar radiation is not blocked by clouds, it is experienced as sunshine, a combination of bright light and radiant heat (Atmospheric). When blocked by clouds or reflected off other objects, sunlight is diffused. Sources estimate a global average of between 164 watts to 340 watts per square meter over a 24-hour day; this figure is estimated by NASA to be about a quarter of Earth's average total solar irradiance.

<span class="mw-page-title-main">Maunder Minimum</span> Period of low solar activity, 1645–1715

The Maunder Minimum, also known as the "prolonged sunspot minimum", was a period around 1645 to 1715 during which sunspots became exceedingly rare. During a 28-year period (1672–1699) within the minimum, observations revealed fewer than 50 sunspots. This contrasts with the typical 40,000–50,000 sunspots seen in modern times over a similar timespan.

<span class="mw-page-title-main">Solar flare</span> Eruption of electromagnetic radiation

A solar flare is a relatively intense, localized emission 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 eruptive solar phenomena. The occurrence of solar flares varies with the 11-year solar cycle.

<span class="mw-page-title-main">Solar maximum</span> Regular period of greatest solar activity

Solar maximum is the regular period of greatest solar activity during the Sun's 11-year solar cycle. During solar maximum, large numbers of sunspots appear, and the solar irradiance output grows by about 0.07%. On average, the solar cycle takes about 11 years to go from one solar maximum to the next, with duration observed varying from 9 to 14 years.

<span class="mw-page-title-main">Solar cycle</span> Periodic change in the Suns activity

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.

<span class="mw-page-title-main">Solar constant</span> Intensity of sunlight or solar constant

The solar constant (GSC) measures the amount of energy received by a given area one astronomical unit away from the Sun. More specifically, it is a flux density measuring mean solar electromagnetic radiation per unit area. It is measured on a surface perpendicular to the rays, one astronomical unit (au) from the Sun.

<span class="mw-page-title-main">Radiative forcing</span> Difference between solar irradiance absorbed by the Earth and energy radiated back to space

Radiative forcing is a concept used in climate science to quantify the change in energy balance in Earth's atmosphere. Various factors contribute to this change in energy balance, such as concentrations of greenhouse gases and aerosols, and changes in surface albedo and solar irradiance. In more technical terms, it is defined as "the change in the net, downward minus upward, radiative flux due to a change in an external driver of climate change." These external drivers are distinguished from feedbacks and variability that are internal to the climate system, and that further influence the direction and magnitude of imbalance. Radiative forcing on Earth is meaningfully evaluated at the tropopause and at the top of the stratosphere. It is quantified in units of watts per square meter, and often summarized as an average over the total surface area of the globe.

<span class="mw-page-title-main">Solar minimum</span> Regular period of least solar activity

Solar minimum is the regular period of least solar activity in the Sun's 11-year solar cycle. During solar minimum, sunspot and solar flare activity diminishes, and often does not occur for days at a time. On average, the solar cycle takes about 11 years to go from one solar minimum to the next, with duration observed varying from 9 to 14 years. The date of the minimum is described by a smoothed average over 12 months of sunspot activity, so identifying the date of the solar minimum usually can only happen 6 months after the minimum takes place.

In solar physics, the Babcock model and its variants describe a mechanism with which they attempt to explain magnetic and sunspot patterns observed on the Sun. It is named after Horace W. Babcock.

<span class="mw-page-title-main">Solar irradiance</span> Measurement of electromagnetic radiation

Solar irradiance is the power per unit area received from the Sun in the form of electromagnetic radiation in the wavelength range of the measuring instrument. Solar irradiance is measured in watts per square metre (W/m2) in SI units.

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.

<span class="mw-page-title-main">Solar cycle 24</span> Solar activity from December 2008 to December 2019

Solar cycle 24 is the most recently completed solar cycle, the 24th since 1755, when extensive recording of solar sunspot activity began. It began in December 2008 with a minimum smoothed sunspot number of 2.2, and ended in December 2019. Activity was minimal until early 2010. It reached its maximum in April 2014 with a 23 months smoothed sunspot number of 81.8. This maximum value was substantially lower than other recent solar cycles, down to a level which had not been seen since cycles 12 to 15 (1878-1923).

<span class="mw-page-title-main">Solar cycle 21</span> Solar activity from March 1976 to September 1986

Solar cycle 21 was the 21st solar cycle since 1755, when extensive recording of solar sunspot activity began. The solar cycle lasted 10.5 years, beginning in March 1976 and ending in September 1986. The maximum smoothed sunspot number observed during the solar cycle was 232.9, in December 1979, and the starting minimum was 17.8. During the minimum transit from solar cycle 21 to 22, there were a total of 273 days with no sunspots. The largest solar flare of this cycle (X15) occurred on July 11, 1978.

<span class="mw-page-title-main">Solar cycle 25</span> Predicted Sun activity 2019 to about 2030

Solar cycle 25 is the current solar cycle, the 25th since 1755, when extensive recording of solar sunspot activity began. It began in December 2019 with a minimum smoothed sunspot number of 1.8. It is expected to continue until about 2030.

Solar observation is the scientific endeavor of studying the Sun and its behavior and relation to the Earth and the remainder of the Solar System. Deliberate solar observation began thousands of years ago. That initial era of direct observation gave way to telescopes in the 1600s followed by satellites in the twentieth century.

<span class="mw-page-title-main">Solar phenomena</span> Natural phenomena within the Suns atmosphere

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

<span class="mw-page-title-main">Solar activity and climate</span> Field of scientific study

Patterns of solar irradiance and solar variation have been a main driver of climate change over the millions to billions of years of the geologic time scale.

References

  1. 1 2 3 4 Hatfield, Miles (2020-05-22). "FAQ: How Does the Solar Cycle Affect Earth's Climate?". NASA . Retrieved 2023-04-20.
  2. "Is the Sun causing global warming?". climate.nasa.gov. Earth Science Communications Team. Archived from the original on 18 January 2024. Retrieved 6 March 2024.
  3. "NASA - SOLAR IRRADIANCE". www.nasa.gov. Retrieved 2023-04-20.
  4. 1 2 3 4 5 6 Kobashi, T.; Box, J. E.; Vinther, B. M.; Goto-Azuma, K.; Blunier, T.; White, J. W. C.; Nakaegawa, T.; Andresen, C. S. (2015-07-28). "Modern solar maximum forced late twentieth century Greenland cooling: SOLAR MAXIMUM FORCED GREENLAND COOLING". Geophysical Research Letters. 42 (14): 5992–5999. doi: 10.1002/2015GL064764 . S2CID   53577049.
  5. 1 2 Lean, J. L. (March 2018). "Estimating Solar Irradiance Since 850 CE". Earth and Space Science. 5 (4): 133–149. Bibcode:2018E&SS....5..133L. doi: 10.1002/2017EA000357 . S2CID   125680439.