دورة شمسية

(تم التحويل من Solar variation)
هذا المقال هو عن دورة البقع الشمسية. إذا كنت تريد دورة تستغرق 28 سنة في التقويم اليولياني، انظر الدورة الشمسية (تقويم).
Line graph showing historical sunspot number count, Maunder and Dalton minima, and the Modern Maximum
تاريخ 400 سنة للبقع الشمسية، يضم Maunder Minimum
"التوقع الحالي للدورة 24 للبقع الشمسية يعطي عدداً مُملـَّس للبقع الشمسية يناهز 69 في أواخر صيف 2013. العدد المملـَّس للبقع الشمسية بلغ 68.9 في أغسطس 2013 ولذلك فالعدد الأقصى الرسمي سيكون على الأقل هو ذلك الرقم. العدد المملـَّس للبقع الشمسية بدأ في الارتفاع مرة أخرى باتجاه تلك القمة الثانية على مدى الأشهر الخمس الأخيرة وقد تجاوزت الآن مستوى القمة الأولى (66.9 في فبراير 2012). العديد من الدورات تتسم بقمتين ولكن هذه الدورة هي الأولى التي تكون فيها القمة الثانية لعدد البقع الشمسية أكبر من القمة الأولى. وحالياً تجاوزنا السنة الخامسة في الدورة رقم 24. حجم (عدد) القع الشمسية المتوقع حالياً والمرصود يجعل هذه الدورة أصغر دورة بقع شمسية منذ الدورة 14 التي كان عددها الأقصى 64.2 في فبراير 1906."[1]

الدورة الشمسية solar cycle أو دورة النشاط المغناطيسي الشمسي هي تغير شبه دوري كل 11 سنة في نشاط الشمس مقاساً بالتغيرات في عدد البقع الشمسية المرصودة على سطح الشمس. والبقع الشمسية تـُرصَد منذ مطلع القرن 17 وسلسلة زمن البقع الشمسية هي أطول سلسلة زمنية (مسجلة) مرصودة باستمرار لأي ظاهرة طبيعية.

ينقلب المجال المغناطيسي للشمس خلال كل دورة شمسية ، ويحدث الانقلاب عندما تقترب دورة البقع الشمسية من الحد الأقصى. مستويات الإشعاع الشمسي وقذف المواد الشمسية، وعدد وحجم البقع الشمسية و الشواظ الشمسية و الحلقة الإكليلية كلها تظهر تقلبًا متزامنًا من نشط الهدوء إلى النشاط مرة أخرى، مع فترة 11 عامًا.

رُصِدت هذه الدورة لقرون بتغيرات في مظهر الشمس وبالظواهر الأرضية مثل auroras. Solar activity, driven both by the sunspot cycle and transient aperiodic processes govern the environment of the Solar System planets by creating space weather and impact space- and ground-based technologies as well as the Earth's atmosphere and also possibly climate fluctuations on scales of centuries and longer.

Understanding and predicting the sunspot cycle remains one of the grand challenges in astrophysics with major ramifications for space science and the understanding of magnetohydrodynamic phenomena elsewhere in the Universe.

Evolution of magnetism on the Sun.

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تعريف

Solar cycles have an average duration of about 11 years. Solar maximum and solar minimum refer respectively to periods of maximum and minimum sunspot counts. Cycles span from one minimum to the next.


التاريخ الرصدي

مقال رئيسي: تاريخ رصد الشمس
صاموِل هاينرش شڤابه (1789–1875). فلكي ألماني، اكتشف الدورة الشمسية عبر أرصاد ممددة للبقع الشمسية
رودلف ڤولف (1816–1893)، فلكي سويسري، قام بإعادة بناء تاريخي للنشاط الشمسي حتى القرن السابع عشر

The solar cycle was discovered in 1843 by صاموِل هاينرش شڤابه, who after 17 years of observations noticed a periodic variation in the average number of sunspots.[2] رودلف ڤولف compiled and studied these and other observations, reconstructing the cycle back to 1745, eventually pushing these reconstructions to the earliest observations of sunspots by Galileo and contemporaries in the early seventeenth century.

Following Wolf's numbering scheme, the 1755–1766 cycle is traditionally numbered "1". Wolf created a standard sunspot number index, the Wolf index, which continues to be used today.

The period between 1645 and 1715, a time of few sunspots,[3] is known as the Maunder minimum, after Edward Walter Maunder, who extensively researched this peculiar event, first noted by Gustav Spörer.

In the second half of the nineteenth century Richard Carrington and Spörer independently noted the phenomena of sunspots appearing at different latitudes at different parts of the cycle.

The cycle's physical basis was elucidated by George Ellery Hale and collaborators, who in 1908 showed that sunspots were strongly magnetized (the first detection of magnetic fields beyond the Earth). In 1919 they showed that the magnetic polarity of sunspot pairs:

  • Is constant throughout a cycle;
  • Is opposite across the equator throughout a cycle;
  • Reverses itself from one cycle to the next.

Hale's observations revealed that the complete magnetic cycle spans two solar cycles, or 22 years, before returning to its original state. However, because nearly all manifestations are insensitive to polarity, the "11-year solar cycle" remains the focus of research. Furthermore, the two halves of the 22-year cycle are typically not identical; the 11-year cycles usually alternate between higher and lower sums of Wolf’s sunspot numbers (the Gnevyshev-Ohl rule).[4]

In 1961 the father-and-son team of Harold and Horace Babcock established that the solar cycle is a spatiotemporal magnetic process unfolding over the Sun as a whole. They observed that the solar surface is magnetized outside of sunspots, that this (weaker) magnetic field is to first order a dipole, and that this dipole undergoes polarity reversals with the same period as the sunspot cycle. Horace's Babcock Model described the Sun's oscillatory magnetic field as having a quasi-steady periodicity of 22 years.[2][5] It covered the oscillatory exchange of energy between toroidal and poloidal solar magnetic field ingredients.

تاريخ الدورة

Reconstruction of solar activity over 11,400 years. Period of equally high activity over 8,000 years ago marked.

Sunspot numbers over the past 11,400 years have been reconstructed using Carbon-14-based dendroclimatology. The level of solar activity beginning in the 1940s is exceptional – the last period of similar magnitude occurred around 9,000 years ago (during the warm Boreal period).[6][7][8] The Sun was at a similarly high level of magnetic activity for only ~10% of the past 11,400 years. Almost all earlier high-activity periods were shorter than the present episode.[7] Fossil records suggest that the Solar cycle has been stable for at least the last 700 million years. For example, the cycle length during the early Permian is estimated to be 10.62 years[9] and similarly in the Neoproterozoic.[10][11]

Solar activity events recorded in radiocarbon. Present period is on right. Values since 1900 not shown.
الأحداث الرئيسية والتواريخ التقريبية
الحدث بدأ انتهى
Homeric minimum[12] 950 BCE 800 BCE
Oort minimum 1040 1080
Medieval maximum 1100 1250
Wolf minimum 1280 1350
Spörer Minimum 1450 1550
Maunder Minimum 1645 1715
Dalton Minimum 1790 1820
Modern Maximum 1900 present

Until 2009 it was thought that 28 cycles had spanned the 309 years between 1699 and 2008, giving an average length of 11.04 years, but research then showed that the longest of these (1784–1799) seems actually to have been two cycles,[13][14] so that the average length is only around 10.7 years. Since observations began cycles as short as 9 years and as long as 14 years have been observed, and in the double cycle of 1784–1799 one of the two component cycles had to be less than 8 years in length. Significant amplitude variations also occur.

A list of historical "grand minima" of solar activity exists.[6]

الدورات، مؤخراً

الدورة 25

There are many, often mutually contradictory predictions,[15] based on different methods, for the forthcoming solar cycle 25, ranging from very weak to moderate magnitude. At present, no definite prediction can be made.

الدورة 24

The current solar cycle began on 4 January 2008,[16] with minimal activity until early 2010.[17][18] It is on track to have the lowest recorded sunspot activity since accurate records began in 1750. The cycle featured a "double-peaked" solar maximum. The first peak reached 99 in 2011 and the second in early 2014 at 101.[19] It appears likely that Cycle 24 will end in mid-2018.[20]

الدورة 23

This cycle lasted 11.6 years, beginning in May 1996 and ending in January 2008. The maximum smoothed sunspot number (monthly number of sunspots averaged over a twelve-month period) observed during the solar cycle was 120.8 (March 2000), and the minimum was 1.7 .[21] A total of 805 days had no sunspots during this cycle.[22][23][24]

الظواهر

مقال رئيسي: Solar phenomena
Because the solar cycle reflects magnetic activity, various magnetically driven solar phenomena follow the solar cycle, including sunspots and coronal mass ejections.

البقع الشمسية

رسم لبقعة شمسية في تأريخ جون من ووستر.
مقال رئيسي: بقعة شمسية

The Sun's apparent surface, the photosphere, radiates more actively when there are more sunspots. Satellite monitoring of solar luminosity revealed a direct relationship between the Schwabe cycle and luminosity with a peak-to-peak amplitude of about 0.1%.[25] Luminosity decreases by as much as 0.3% on a 10-day timescale when large groups of sunspots rotate across the Earth's view and increase by as much as 0.05% for up to 6 months due to faculae associated with large sunspot groups.[26]

The best information today comes from SOHO (a cooperative project of the European Space Agency and NASA), such as the MDI magnetogram, where the solar "surface" magnetic field can be seen.

As each cycle begins, sunspots appear at mid-latitudes, and then move closer and closer to the equator until a solar minimum is reached. This pattern is best visualized in the form of the so-called butterfly diagram. Images of the Sun are divided into latitudinal strips, and the monthly-averaged fractional surface of sunspots is calculated. This is plotted vertically as a color-coded bar, and the process is repeated month after month to produce this time-series diagram.

The sunspot butterfly diagram. This modern version is constructed (and regularly updated) by the solar group at NASA Marshall Space Flight Center.

While magnetic field changes are concentrated at sunspots, the entire sun undergoes analogous changes, albeit of smaller magnitude.

Time vs. solar latitude diagram of the radial component of the solar magnetic field, averaged over successive solar rotation. The "butterfly" signature of sunspots is clearly visible at low latitudes. Diagram constructed (and regularly updated) by the solar group at NASA Marshall Space Flight Center.


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Coronal mass ejection

مقال رئيسي: Coronal mass ejection
The solar magnetic field structures the corona, giving it its characteristic shape visible at times of solar eclipses. Complex coronal magnetic field structures evolve in response to fluid motions at the solar surface, and emergence of magnetic flux produced by dynamo action in the solar interior. For reasons not yet understood in detail, sometimes these structures lose stability, leading to coronal mass ejections into interplanetary space, or flares, caused by sudden localized release of magnetic energy driving emission of ultraviolet and X-ray radiation as well as energetic particles. These eruptive phenomena can have a significant impact on Earth's upper atmosphere and space environment, and are the primary drivers of what is now called space weather.

The occurrence frequency of coronal mass ejections and flares is strongly modulated by the cycle. Flares of any given size are some 50 times more frequent at solar maximum than at minimum. Large coronal mass ejections occur on average a few times a day at solar maximum, down to one every few days at solar minimum. The size of these events themselves does not depend sensitively on the phase of the solar cycle. A case in point are the three large X-class flares that occurred in December 2006, very near solar minimum; an X9.0 flare on Dec 5 stands as one of the brightest on record.[27]

الأنماط

An overview of three solar cycles shows the relationship between the sunspot cycle, galactic cosmic rays, and the state of our near-space environment.[28]

The Waldmeier effect names the observation that cycles with larger maximum amplitudes tend to take less time to reach their maxima than cycles with smaller amplitudes;[29] maximum amplitudes are negatively correlated to the lengths of earlier cycles, aiding prediction.[30]

Solar maxima and minima also exhibit fluctuations at time scales greater than solar cycles. Increasing and decreasing trends can continue for periods of a century or more.

The Schwabe Cycle is thought to be an amplitude modulation of the 87 year (70–100 year) Gleissberg cycle, named after Wolfgang Gleißberg.[4][31][32] The Gleisberg cycle implied that the next solar cycle have a maximum smoothed sunspot number of about 145±30 in 2010 (instead 2010 was just after the cycle's solar minimum) and that the following cycle have a maximum of about 70±30 in 2023.[33]

Associated centennial variations in magnetic fields in the Corona and Heliosphere have been detected using Carbon-14 and beryllium-10 cosmogenic isotopes stored in terrestrial reservoirs such as ice sheets and tree rings[34] and by using historic observations of Geomagnetic storm activity, which bridge the time gap between the end of the usable cosmogenic isotope data and the start of modern satellite data.[35]

These variations have been successfully reproduced using models that employ magnetic flux continuity equations and observed sunspot numbers to quantify the emergence of magnetic flux from the top of the solar atmosphere and into the Heliosphere,[36] showing that sunspot observations, geomagnetic activity and cosmogenic isotopes offer a convergent understanding of solar activity variations.

2,300 year Hallstatt solar variation cycles.

الدورات المفترضة

Periodicity of solar activity with periods longer than the sunspot cycle has been proposed,[4] including:

The 210 year Suess cycle[32] (a.k.a. "de Vries cycle", named after Hans Eduard Suess and Hessel De Vries respectively) is recorded from radiocarbon studies, although "little evidence of the Suess Cycle" appears in the 400-year sunspot record.[4]

The Hallstatt cycle (named after a cool and wet period in Europe when glaciers advanced) is hypothesized to extend for approximately 2,400 years.[37][38][39][40]

An as yet unnamed cycle may extend over 6,000 years.[41]

In carbon-14 cycles of 105, 131, 232, 385, 504, 805 and 2,241 years have been observed, possibly matching cycles derived from other sources.[42] Damon and Sonett[43] proposed carbon 14-based medium- and short-term variations of periods 208 and 88 years; as well as suggesting a 2300-year radiocarbon period that modulates the 208-year period.[44]

During the Upper Permian 240 million years ago, mineral layers created in the Castile Formation show cycles of 2,500 years.[45]

المجال المغناطيسي الشمسي

The Sun's magnetic field structures its atmosphere and outer layers all the way through the corona and into the solar wind. Its spatiotemporal variations lead to various measurable solar phenomena. Other solar phenomena are closely related to the cycle, which serves as the energy source and dynamical engine for the former.

الآثار

الشمسية

Activity cycles 21, 22 and 23 seen in sunspot number index, TSI, 10.7cm radio flux, and flare index. The vertical scales for each quantity have been adjusted to permit overplotting on the same vertical axis as TSI. Temporal variations of all quantities are tightly locked in phase, but the degree of correlation in amplitudes is variable to some degree.

مغناطيسية الأسطح

Sunspots eventually decay, releasing magnetic flux in the photosphere. This flux is dispersed and churned by turbulent convection and solar large-scale flows. These transport mechanisms lead to the accumulation of magnetized decay products at high solar latitudes, eventually reversing the polarity of the polar fields (notice how the blue and yellow fields reverse in the Hathaway/NASA/MSFC graph above).

The dipolar component of the solar magnetic field reverses polarity around the time of solar maximum and reaches peak strength at the solar minimum.

الفضاء

المركبات الفضائية

CMEs (coronal mass ejections) produce a radiation flux of high-energy protons, sometimes known as solar cosmic rays. These can cause radiation damage to electronics and solar cells in satellites. Solar proton events also can cause single-event upset (SEU) events on electronics; at the same, the reduced flux of galactic cosmic radiation during solar maximum decreases the high-energy component of particle flux.

CME radiation is dangerous to astronauts on a space mission who are outside the shielding produced by the Earth's magnetic field. Future mission designs (e.g., for a Mars Mission) therefore incorporate a radiation-shielded "storm shelter" for astronauts to retreat to during such an event.

Gleißberg developed a CME forecasting method that relies on consecutive cycles.[46]

On the positive side, the increased irradiance during solar maximum expands the envelope of the Earth's atmosphere, causing low-orbiting space debris to re-enter more quickly.


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فيض الآشعة الكونية المجرّية

The outward expansion of solar ejecta into interplanetary space provides overdensities of plasma that are efficient at scattering high-energy cosmic rays entering the solar system from elsewhere in the galaxy. The frequency of solar eruptive events is modulated by the cycle, changing the degree of cosmic ray scattering in the outer solar system accordingly. As a consequence, the cosmic ray flux in the inner solar system is anticorrelated with the overall level of solar activity.[47] This anticorrelation is clearly detected in cosmic ray flux measurements at the Earth's surface.

Some high-energy cosmic rays entering Earth's atmosphere collide hard enough with molecular atmospheric constituents to cause occasionally nuclear spallation reactions. Fission products include radionuclides such as 14C and 10Be that settle on the Earth's surface. Their concentration can be measured in ice cores, allowing a reconstruction of solar activity levels into the distant past.[48] Such reconstructions indicate that the overall level of solar activity since the middle of the twentieth century stands amongst the highest of the past 10,000 years, and that epochs of suppressed activity, of varying durations have occurred repeatedly over that time span.

الغلاف الجوي

Solar irradiance

مقال رئيسي: Solar irradiance
The total solar irradiance (TSI) is the amount of solar radiative energy incident on the Earth's upper atmosphere. TSI variations were undetectable until satellite observations began in late 1978. A series of radiometers were launched on satellites from the 1970s to the 2000s.[49] TSI measurements varied from 1360 to 1370 W/m2 across ten satellites. One of the satellites, the ACRIMSAT was launched by the ACRIM group. The controversial 1989–1991 "ACRIM gap" between non-overlapping ACRIM satellites was interpolated by the ACRIM group into a composite showing +0.037%/decade rise. Another series based on the ACRIM data is produced by the PMOD group and shows a −0.008%/decade downward trend.[50] This 0.045%/decade difference impacts climate models.

Solar irradiance varies systematically over the cycle,[51] both in total irradiance and in its relative components (UV vs visible and other frequencies). The solar luminosity is an estimated 0.07 percent brighter during the mid-cycle solar maximum than the terminal solar minimum. Photospheric magnetism appears to be the primary cause (96%) of 1996–2013 TSI variation.[52] The ratio of ultraviolet to visible light varies.[53]

TSI varies in phase with the solar magnetic activity cycle[54] with an amplitude of about 0.1% around an average value of about 1361.5 W/m2[55] (the "solar constant"). Variations about the average of up to −0.3% are caused by large sunspot groups and of +0.05% by large faculae and the bright network on a 7-10-day timescale[56] (see TSI variation graphics).[57] Satellite-era TSI variations show small but detectable trends.[58][59]

TSI is higher at solar maximum, even though sunspots are darker (cooler) than the average photosphere. This is caused by magnetized structures other than sunspots during solar maxima, such as faculae and active elements of the "bright" network, that are brighter (hotter) than the average photosphere. They collectively overcompensate for the irradiance deficit associated with the cooler, but less numerous sunspots. The primary driver of TSI changes on solar rotational and sunspot cycle timescales is the varying photospheric coverage of these radiatively active solar magnetic structures.[بحاجة لمصدر]

Energy changes in UV irradiance involved in production and loss of ozone have atmospheric effects. The 30 HPa Atmospheric pressure level changed height in phase with solar activity during solar cycles 20–23. UV irradiance increase caused higher ozone production, leading to stratospheric heating and to poleward displacements in the stratospheric and tropospheric wind systems.[60]

إشعاع الموجات القصيرة

A solar cycle: a montage of ten years' worth of Yohkoh SXT images, demonstrating the variation in solar activity during a sunspot cycle, from after August 30, 1991, to September 6, 2001. Credit: the Yohkoh mission of ISAS (Japan) and NASA (US).

With a temperature of 5870 K, the photosphere emits a proportion of radiation in the extreme ultraviolet (EUV) and above. However, hotter upper layers of the Sun's atmosphere (chromosphere and corona) emit more short-wavelength radiation. Since the upper atmosphere is not homogeneous and contains significant magnetic structure, the solar ultraviolet (UV), EUV and X-ray flux varies markedly over the cycle.

The photo montage to the left illustrates this variation for soft X-ray, as observed by the Japanese satellite Yohkoh from after August 30, 1991, at the peak of cycle 22, to September 6, 2001, at the peak of cycle 23. Similar cycle-related variations are observed in the flux of solar UV or EUV radiation, as observed, for example, by the SOHO or TRACE satellites.

Even though it only accounts for a minuscule fraction of total solar radiation, the impact of solar UV, EUV and X-ray radiation on the Earth's upper atmosphere is profound. Solar UV flux is a major driver of stratospheric chemistry, and increases in ionizing radiation significantly affect ionosphere-influenced temperature and electrical conductivity.

الفيض الراديوي الشمسي

Emission from the Sun at centimetric (radio) wavelength is due primarily to coronal plasma trapped in the magnetic fields overlying active regions.[61] The F10.7 index is a measure of the solar radio flux per unit frequency at a wavelength of 10.7 cm, near the peak of the observed solar radio emission. F10.7 is often expressed in SFU or solar flux units (1 SFU = 10−22 W m−2 Hz−1). It represents a measure of diffuse, nonradiative coronal plasma heating. It is an excellent indicator of overall solar activity levels and correlates well with solar UV emissions.

Sunspot activity has a major effect on long distance radio communications, particularly on the shortwave bands although medium wave and low VHF frequencies are also affected. High levels of sunspot activity lead to improved signal propagation on higher frequency bands, although they also increase the levels of solar noise and ionospheric disturbances. These effects are caused by impact of the increased level of solar radiation on the ionosphere.

10.7 cm solar flux could interfere with point-to-point terrestrial communications.[62]

السـُحـُب

The cosmic ray changes over the cycle potentially have significant atmospheric effects. Speculations about cosmic rays include:

  • Changes in ionization affect the aerosol abundance that serves as the condensation nucleus for cloud formation.[63] During solar minima more cosmic rays reach Earth, potentially creating ultra-small aerosol particles as precursors to Cloud condensation nuclei.[64] Clouds formed from greater amounts of condensation nuclei are brighter, longer lived and likely to produce less precipitation.
  • A change in cosmic rays could cause an increase in certain types of clouds, affecting Earth's albedo.[بحاجة لمصدر]
  • It was proposed that, particularly at high latitudes, cosmic ray variation may impact terrestrial low altitude cloud cover (unlike a lack of correlation with high altitude clouds), partially influenced by the solar-driven interplanetary magnetic field (as well as passage through the galactic arms over longer timeframes),[65][66][67][68] but this hypothesis was not confirmed.[69]

Later papers claimed that production of clouds via cosmic rays could not be explained by nucleation particles. Accelerator results failed to produce sufficient, and sufficiently large, particles to result in cloud formation;[70][71] this includes observations after a major solar storm.[72] Observations after Chernobyl do not show any induced clouds.[73]

الأرضية

العضيات

The impact of the solar cycle on living organisms has been investigated (see chronobiology). Some researchers claim to have found connections with human health.[74]

The amount of ultraviolet UVB light at 300 nm reaching the Earth varies by as much as 400% over the solar cycle due to variations in the protective ozone layer. In the stratosphere, ozone is continuously regenerated by the splitting of O2 molecules by ultraviolet light. During a solar minimum, the decrease in ultraviolet light received from the Sun leads to a decrease in the concentration of ozone, allowing increased UVB to reach the Earth's surface.[75]

الاتصالات الراديوية

مقال رئيسي: Skywave

Skywave modes of radio communication operate by bending (refracting) radio waves (electromagnetic radiation) through the Ionosphere. During the "peaks" of the solar cycle, the ionosphere becomes increasingly ionized by solar photons and cosmic rays. This affects the propagation of the radio wave in complex ways that can either facilitate or hinder communications. Forecasting of skywave modes is of considerable interest to commercial marine and aircraft communications, amateur radio operators and shortwave broadcasters. These users occupy frequencies within the High Frequency or 'HF' radio spectrum that are most affected by these solar and ionospheric variances. Changes in solar output affect the maximum usable frequency, a limit on the highest frequency usable for communications.

المناخ

Both long-term and short-term variations in solar activity are theorized to affect global climate, but it has proven challenging to quantify the link between solar variation and climate.[76]

Early research attempted to correlate weather with limited success,[77] followed by attempts to correlate solar activity with global temperature. The cycle also impacts regional climate. Measurements from the SORCE's Spectral Irradiance Monitor show that solar UV variability produces, for example, colder winters in the U.S. and northern Europe and warmer winters in Canada and southern Europe during solar minima.[78]

Three hypothetical mechanisms mediate solar variations' climate impacts:

  • Total solar irradiance ("Radiative forcing").
  • Ultraviolet irradiance. The UV component varies by more than the total, so if UV were for some (as yet unknown) reason having a disproportionate effect, this might affect climate.
  • Solar wind-mediated galactic cosmic ray changes, which may affect cloud cover.

The sunspot cycle variation of 0.1% has small but detectable effects on the Earth’s climate.[79][80][81] Camp and Tung suggest that solar irradiance correlates with a variation of 0.18 K ±0.08 K (0.32 °F ±0.14 °F) in measured average global temperature between solar maximum and minimum.[82]

Other statistically significant effects have been reported. One study found a relationship with wheat prices[83], and another found a correlation with the flow of water in the Paraná River.[84] Eleven-year cycles have been found in tree-ring thicknesses[9] and layers at the bottom of a lake[10] hundreds of millions of years ago.

The current scientific consensus, most specifically that of the IPCC, is that solar variations do play a marginal role in driving global warming,[76] since the measured magnitude of recent solar variation is much smaller than the forcing due to greenhouse gases.[85] Also, solar activity in the 2010s was not higher than in the 1950s (see above), whereas global warming had risen markedly. Otherwise, the level of understanding of solar impacts on weather is low.[86]

Solar cycle also affects the orbital decay of Low Earth Orbiting (LEO) objects by affecting the density at the upper thermospheric levels. [87]

دينامو شمسي

مقال رئيسي: دينامو شمسي

The 11-year sunspot cycle is half of a 22-year Babcock–Leighton solar 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 Convection zone forces emergence of the toroidal magnetic field through the photosphere, giving rise to pairs of sunspots, roughly aligned east–west with opposite magnetic polarities. The magnetic polarity of sunspot pairs alternates every solar cycle, a phenomenon known as the Hale cycle.[88][89]

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. At solar minimum, the toroidal field is, correspondingly, at minimum strength, sunspots are relatively rare and the poloidal field is at maximum strength. During the next cycle, differential rotation converts magnetic energy back from the poloidal to the toroidal field, 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 in the polarity of the Sun's large-scale magnetic field.[90][91]

Although the tachocline has long been thought to be the key to generating the Sun's large-scale magnetic field, recent research has questioned this assumption. Radio observations of brown dwarfs have indicated that they also maintain large-scale magnetic fields and may display cycles of magnetic activity. The Sun has a radiative core surrounded by a convective envelope, and at the boundary of these two is the tachocline. However, brown dwarfs lack radiative cores and tachoclines. Their structure consists of a solar-like convective envelope that exists from core to surface. Since they lack a tachocline yet still display solar-like magnetic activity, it has been suggested that solar magnetic activity is only generated in the convective envelope.[92]

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