لکه خورشیدی

نگاره‌ای از لکه‌های خورشیدی در تاریخ ۲۰۰۴-۰۶-۲۲

لکه‌های سطح خورشید در نقشهٔ ساموئل دان

لکهٔ خورشیدی رویدادی موقت بر روی سطح خورشید (نورسپهر/فوتوسفر) است که به‌صورت لکه‌هایی تاریک‌تر از نواحی اطراف آنها به‌وسیلهٔ فعالیت‌های شدید شار مغناطیسی که مانع از انتقال گرما می‌شود به وجود می‌آید. این لکه‌ها به علت کاهش درجهٔ حرارت سطح خورشید در آن ناحیه‌ها به وجود می‌آیند. لکه‌های خورشیدی دارای قطرهایی به ابعاد ۱۶ کیلومتر (۱۰ مایل) تا ۱۶۰٬۰۰۰ کیلومتر (۱۰۰٬۰۰۰ مایل) هستند و بزرگ‌ترین آن‌ها بدون تلسکوپ هم قابل مشاهده است. اگرچه این ناحیه‌ها هنوز درجهٔ حرارتی در حدود ۳٬۰۰۰–۴٬۵۰۰ کلوین دارند، تفاوت دمای این ناحیه‌ها با مواد پیرامون؛ حدود ۵٬۸۰۰ کلوین، به آن‌ها اجازه می‌دهد تا به وضوح به عنوان لکه‌های سیاه دیده شوند، همچون بدنه‌ای که از شدت گرما سیاه شده باشد (تقریباً نزدیک نورسپهر) این تابعی از T (دما) به توان چهارم است. اگر یک لکه خورشیدی از نورسپهر/فوتوسفر جدا شود می‌تواند قوس الکتریکی درخشانی را به وجود بیاورد.

لکهٔ خورشیدی، در حین ظاهر شدن از فعالیت‌های شدید مغناطیسی، میزبان آثار دیگری مانند تاج‌های خورشیدی و رخدادهای قطع ارتباط نیز هستند. بیشتر شراره‌های خورشیدی و پس‌زنی تودهٔ تاج سرچشمه در فعالیت‌های مغناطیسی پیرامون منطقهٔ گروه‌های لکه قابل رؤیت خورشید دارند. پدیده‌های مشابهی که به‌طور غیرمستقیم در ستاره‌ها نیز رصد شده‌اند عموماً لکه‌های ستاره‌ای نامیده می‌شوند و در دو نوع روشن و تاریک اندازه‌گیری شده‌اند. این لکه دائمی نیست

نحوهٔ کشف و مشخصات

لکه‌های خورشیدی در خورشیدگرفتگی ۱ خرداد ۱۳۹۱

پیش از سال ۱۶۱۵ میلادی اروپاییان عقیده داشتند که خورشید یک کرهٔ تابناک و بی‌لکه باشد.

در آن سال گالیله پیک نجومی خود را چاپ کرد که در آن وجود لکه‌های تاریک (لکه‌های خورشیدی) در سطح خورشید را گزارش کرد و نشان داد که لکه‌های خورشیدی پدیده‌های شیدسپهری (سطح مرئی خورشید) می‌باشند؛ که از اطراف شیدسپهر تاریک‌تر هستند. تاریک‌ترین قسمت یعنی ناحیهٔ مرکزی تمام سایه را می‌سازد. لکه‌های خورشیدی کوچک از روزنه‌هایی که بزرگ‌تر از سطوح تاریک معمول میان دانه‌های روشن هستند گسترش می‌یابند. اگر چه بیشتر روزنه‌ها و لکه‌های کوچک خیلی زود تجزیه می‌شوند اما بعضی از آن‌ها به لکه‌های واقعی عظیم تبدیل می‌گردند بزرگ‌ترین لکهٔ تاریک دارای قطر تمام سایه ۳۰٬۰۰۰ کیلومتر و قطرهای ناحیهٔ نیم‌سایه بیشتر از دو برابر این مقدار است. از این رو گاهی هنگام غروب آفتاب که خورشید رنگ پریده می‌گردد می‌توان بدون نیاز به تلسکوپ هم به وجود این لکه‌ها پی برد.

هر لکه از دو قسمت تشکیل می‌شود. یک قسمت مرکزی که رنگ آن تیره است و دیگری اطراف لکه که رنگ آن نسبت به مرکز روشن‌تر است. ظهور هر لکه در سطح خورشید موقتی است و با ایجاد و وسعت عمل آن در یک مدت زمانی به تدریج محو می‌شود. نحوهٔ از میان رفتن آن به این ترتیب است که روشنی اطراف لکه، به تدریج هستهٔ آن را احاطه کرده و به مرکز نزدیک می‌شود و کاملاً منطقهٔ تیره‌رنگ را نابود می‌کند.

اما بر طبق اسناد و مدارک ثابت‌شده اکنون آشکار است که منجمان چینی لااقل در سال 28 قبل از میلاد آنها را رصد کرده بودند و به احتمالی برهمن‌های مُغ یعنی بازماندگان سیستانی‌های آفتاب‌پرست، منجمان چینی را در این امر راهنما، آموزگار و مددکار بوده‌اند.

در مورد لکه‌های خورشیدی نظرهای گوناگونی ارائه شده‌است که مهم‌ترین آن‌ها نظریهٔ اورشید دانشمند معروف سوئدی است. بر اساس این نظریه، قسمتی از داخل خورشید، به شکل یک جریان به سمت خارج آن حرکت می‌کند و پس از رسیدن به سطح، مانند چتری پراکنده می‌شود و چون بر اثر این عمل فشار و حرارت آن کاسته می‌شود، کمی فشرده و سرد گشته و به شکل لکه‌های تیره‌رنگی در سطح خورشید باقی می‌ماند و به تدریج از میان می‌رود.

مهم‌ترین مشخصهٔ لکهٔ خورشیدی میدان مغناطیسی آن می‌باشد؛ که از حدود ۰٫۱ T تا میدان‌های قویتر ۰٫۴ T اندازه‌گیری شده‌اند و باعث می‌شوند از انتقال انرژی به شیدسپهر از طریق جابجایی، جلوگیری شود. از این روست که لکهٔ خورشیدی سردتر از محیط اطرافش می‌باشد. یک لک خورشیدی دارای قطبش مغناطیسی می‌باشد که لکه‌ها را در دو سوی قطب مغناطیسی جمع می‌کند اما ممکن است استثنائاتی وجود داشته باشد که ناحیهٔ مغناطیس دوم پراکنده باشد و فقط یک لک خورشیدی دیده شود.

تعداد لکه‌های خورشیدی متأثر از زمان است و با زمان تغییر می‌کند و برای بیشترین و کمترین تعداد لکه‌ها یک چرخه‌ای به‌طور متوسط یازده سال را در نظر گرفته‌اند.

وضع خورشید همیشه مانند ۲۰۰ سال گذشته یکنواخت نبوده‌است. بین سال‌های ۱۶۴۵ و ۱۷۱۵ هیچ لکهٔ خورشیدی ثبت نشده‌است!

در خلال حداقل لکه‌های خورشیدی طوفان‌های مغناطیسی و جلوه‌های شفقی که معمولاً در کشورهای اروپای شمالی فراوانند در طی این دوره تناوب ۷۰ ساله واقعاً ناپدید شدند. در سال ۱۷۱۵ که فعالیت‌های خورشیدی مجدداً ظاهر شدند، جلوه‌های شفق در مکان‌هایی مثل استکهلم و کپنهاگ باعث نگرانی شدند.

بیش از ۵۰ سال روی رابطهٔ میان چرخهٔ ۱۱ ساله لکه خورشیدی و محیط زمین مطالعه شده‌است. هسل دوریس روی لایه‌های حلقوی تنه درختان که به صورت ۲۰ تایی تاریخگذاری شده بودند، یک تغییر چرخه‌ای در رشد درختان کشف کرد. طی هر دهه یا دو دهه رشد سالانه درختان آهنگی تند و سپس آهنگی کند را داشت. در آخر نیمه قرن ۱۷ این تغییر چرخه همیشگی وجود نداشت این دوره تناوب متناظر با کمینه ماندر در دوره لکه خورشیدی است. مطالعات نشان داده‌است که در ۵۰۰۰ سال گذشته فعالیت خورشیدی مانند کمینه ماندر با دوازده نوسان همراه بوده‌است. مطالعات اخیر نشان داده‌اند که اثرات مستقیم دوره لکه خورشیدی در هوای روز اندک است و لیکن تغییرا ت بلند مدت فعالیت خورشیدی ممکن است در آب و هوای زمین اثر بگذارد. کمینه ماندر در اواخر قرن ۱۷ با بدترین سرمای عصر یخبندان کوچک که اروپا را فلج کرد مصادف شد. رابطه بین فعالیت خورشیدی و محیط زمین مسئله مشکلی است و اغلب با بحث‌های گرم همراه است؛ ولی آنقدر مهم است که نمی‌توان از آن چشم پوشی کرد.

تغییر عرض جغرافیایی

توزیع لکه‌های خورشیدی در عرض جغرافیایی خورشید به طریق به خصوصی در خلال چرخه ۱۱ ساله تعداد لکه خورشیدی تغییر می‌کند. لکه‌های خورشیدی در آغاز یک چرخه در عرض‌های جغرافیایی بالا (۳۵_+) درجه قرار می‌گیرند. بیشتر لکه‌ها در نزدیکی عرض ۱۵ _+ درجه در لت بیشینه خود و چند لکه در انتهای چرخه خوشه نزدیک ۸۰ _+ درجه واقع می‌شوند. تعداد کمی از لکه‌های خورشیدی را حتی می‌توان در عرض جغرافیایی بالاتر از ۴۵_+درجه مشاهده کرد. زمان حیات یک لک خورشیدی از چند روز (برای لکه‌های کوچک) تا چند ماه (برای لکه‌های بزرگ) طول می‌کشد. در حقیقت یک لکه خورشیدی در همان عرض جغرافیایی که متولد شده از بین می‌رود. (مشخصه‌ای که به ما امکان می‌دهد تا چرخش خورشیدی را تعیین کنیم) آنچه که اتفاق می‌افتد این چنین است. همان‌طور که چرخه پیشرفت می‌کند، لکه‌های جدید حتی در عرض‌های جغرافیایی پا یین ظاهر می‌شوند. اولین لکه‌های عرض جغرافیایی بالا از یک چرخه حتی قبل از آخرین لکه‌های عرض جغرافیایی پایین از چرخه قبلی ظاهر می‌شوند. منشأ گرمای خورشید واکنش‌های هسته‌ای است. در این واکنش هیدروژن به هلیوم تبدیل می‌شود و گرمای فراوانی حاصل می‌شود.

نگارخانه

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منابع

• مشارکت‌کنندگان ویکی‌پدیا. «Sun spot». در دانشنامهٔ ویکی‌پدیای انگلیسی، بازبینی‌شده در ۶ اکتبر ۲۰۰۹.
• نجوم واختر فیزیک مقدماتی _جلد اول فیزیک فضا _ زیلیک و اسمیت _ترجمه دکتر تقی عدالتی و جمشید قنبر
• درسهایی از ستاره‌شناسی _ گرد آوری مدرسه ستاره‌شناسی و علوم دریایی مریلند_ ترجمه امیر خداوردیخان

For other uses, see Sunspot (disambiguation).

• Top: active region 2192 in 2014 containing the largest sunspot of solar cycle 24 and active region 1302 in September 2011.
• Middle: sunspot close-up in the visible spectrum (left) and another sunspot in UV, taken by the TRACE observatory.
• Bottom: a large group of sunspots stretching about 320,000 km (200,000 mi) across.

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.

Individual sunspots or groups of sunspots may last anywhere from a few days to a few months, but eventually decay. Sunspots expand and contract as they move across the surface of the Sun, with diameters ranging from 16 km (10 mi) to 160,000 km (100,000 mi). Larger sunspots can be visible from Earth without the aid of a telescope. They may travel at relative speeds, or proper motions, of a few hundred meters per second when they first emerge.

Indicating intense magnetic activity, sunspots accompany other active region phenomena such as coronal loops, prominences, and reconnection events. Most solar flares and coronal mass ejections originate in these magnetically active regions around visible sunspot groupings. Similar phenomena indirectly observed on stars other than the Sun are commonly called starspots, and both light and dark spots have been measured.

History

For broader coverage of this topic, see Solar observation.

The earliest record of sunspots is found in the Chinese I Ching, completed before 800 BC. The text describes that a dou and mei were observed in the sun, where both words refer to a small obscuration. The earliest record of a deliberate sunspot observation also comes from China, and dates to 364 BC, based on comments by astronomer Gan De (甘德) in a star catalogue. By 28 BC, Chinese astronomers were regularly recording sunspot observations in official imperial records.

The first clear mention of a sunspot in Western literature is circa 300 BC, by ancient Greek scholar Theophrastus, student of Plato and Aristotle and successor to the latter.

The first drawings of sunspots were made by English monk John of Worcester in December 1128.

Sunspots were first observed telescopically in December 1610 by English astronomer Thomas Harriot. His observations were recorded in his notebooks and were followed in March 1611 by observations and reports by Frisian astronomers Johannes and David Fabricius. After Johannes Fabricius' death at the age of 29, his reports remained obscure and were eclipsed by the independent discoveries of and publications about sunspots by Christoph Scheiner and Galileo Galilei. Galileo likely began telescopic sunspot observations around the same time as Harriot; however, Galileo's records did not start until 1612.

In the early 19th Century, William Herschel was one of the first to equate sunspots with heating and cooling on Earth and believed that certain features of sunspots would indicate increased heating on Earth. During his recognition of solar behavior and hypothesized solar structure, he inadvertently picked up the relative absence of sunspots from July 1795 to January 1800 and was perhaps the first to construct a past record of observed or missing sunspots. From this he found that the absence of sunspots coincided with high wheat prices in England. The president of the Royal Society commented that the upward trend in wheat prices was due to monetary inflation. Years later scientists such as Richard Carrington in 1865 and John Henry Poynting in 1884 tried and failed to find a connection between wheat prices and sunspots, and modern analysis finds that there is no statistically significant correlation between wheat prices and sunspot numbers.

Physics

Morphology

A decaying sunspot shown over the course of two hours. The umbra is separated into two pieces within the penumbra by a light bridge. Solar pores are also visible to the left of the penumbra.

Sunspots have two main structures: a central umbra and a surrounding penumbra. The umbra is the darkest region of a sunspot and is where the magnetic field is strongest and approximately vertical, or normal, to the Sun's surface, or photosphere. The umbra may be surrounded completely or only partially by a brighter region known as the penumbra. The penumbra is composed of radially elongated structures known as penumbral filaments and has a more inclined magnetic field than the umbra. Within sunspot groups, multiple umbrae may be surrounded by a single, continuous penumbra.

The temperature of the umbra is roughly 3,000–4,500 K (2,700–4,200 °C), in contrast to the penumbra at about 5,780 K (5,500 °C) leaving sunspots clearly visible as dark spots. This is because the luminance of a heated black body (closely approximated by the photosphere) at these temperatures varies greatly with temperature. Isolated from the surrounding photosphere, a single sunspot would shine brighter than the full moon, with a crimson-orange color.

In some forming and decaying sunspots, relatively narrow regions of bright material appear penetrating into or completely dividing an umbra. These formations, referred to as light bridges, have been found to have a weaker, more tilted magnetic field compared to the umbra at the same height in the photosphere. Higher in the photosphere, the light bridge magnetic field merges and becomes comparable to that of the umbra. Gas pressure in light bridges has also been found to dominate over magnetic pressure, and convective motions have been detected.

The Wilson effect implies that sunspots are depressions on the Sun's surface.

Lifecycle

The emergence and evolution of a sunspot group over a period of two weeks

The appearance of an individual sunspot may last anywhere from a few days to a few months, though groups of sunspots and their associated active regions tend to last weeks or months. Sunspots expand and contract as they move across the surface of the Sun, with diameters ranging from 16 km (10 mi) to 160,000 km (100,000 mi).

Formation

Although the details of sunspot formation are still a matter of ongoing research, it is widely understood that they are the visible manifestations of magnetic flux tubes in the Sun's convective zone projecting through the photosphere within active regions. Their characteristic darkening occurs due to this strong magnetic field inhibiting convection in the photosphere. As a result, the energy flux from the Sun's interior decreases, and with it, surface temperature, causing the surface area through which the magnetic field passes to look dark against the bright background of photospheric granules.

Sunspots initially appear in the photosphere as small darkened spots lacking a penumbra. These structures are known as solar pores. Over time, these pores increase in size and move towards one another. When a pore gets large enough, typically around 3,500 km (2,000 mi) in diameter, a penumbra will begin to form.

Decay

Magnetic pressure should tend to remove field concentrations, causing the sunspots to disperse, but sunspot lifetimes are measured in days to weeks. In 2001, observations from the Solar and Heliospheric Observatory (SOHO) using sound waves traveling below the photosphere (local helioseismology) were used to develop a three-dimensional image of the internal structure below sunspots; these observations show that a powerful downdraft underneath each sunspot, forms a rotating vortex that sustains the concentrated magnetic field.

Solar cycle

Main article: Solar cycle

Butterfly diagram showing paired Spörer's law behavior

The full solar disk over the course of 13 days during the rise of solar cycle 24

Solar cycles last typically about eleven years, varying from just under 10 to just over 12 years. Over the solar cycle, sunspot populations increase quickly and then decrease more slowly. The point of highest sunspot activity during a cycle is known as solar maximum, and the point of lowest activity as solar minimum. This period is also observed in most other solar activity and is linked to a variation in the solar magnetic field that changes polarity with this period.

Early in the cycle, sunspots appear at higher latitudes and then move towards the equator as the cycle approaches maximum, following Spörer's law. Spots from two sequential cycles co-exist for several years during the years near solar minimum. Spots from sequential cycles can be distinguished by direction of their magnetic field and their latitude.

The Wolf number sunspot index counts the average number of sunspots and groups of sunspots during specific intervals. The 11-year solar cycles are numbered sequentially, starting with the observations made in the 1750s.

George Ellery Hale first linked magnetic fields and sunspots in 1908. Hale suggested that the sunspot cycle period is 22 years, covering two periods of increased and decreased sunspot numbers, accompanied by polar reversals of the solar magnetic dipole field. Horace W. Babcock later proposed a qualitative model for the dynamics of the solar outer layers. The Babcock Model explains that magnetic fields cause the behavior described by Spörer's law, as well as other effects, which are twisted by the Sun's rotation.

Longer-period trends

Main article: Solar cycle § Cycle history

Sunspot numbers also change over long periods. For example, during the period known as the modern maximum from 1900 to 1958 the solar maxima trend of sunspot count was upwards; for the following 60 years the trend was mostly downwards. Overall, the Sun was last as active as the modern maximum over 8,000 years ago.

Sunspot number is correlated with the intensity of solar radiation over the period since 1979, when satellite measurements became available. The variation caused by the sunspot cycle to solar output is on the order of 0.1% of the solar constant (a peak-to-trough range of 1.3 W·m⁻² compared with 1366 W·m⁻² for the average solar constant).

400-year history of sunspot numbers, showing Maunder and Dalton minima, and the Modern Maximum (left) and 11,000-year sunspot reconstruction showing a downward trend over 2000 BC – 1600 AD followed by the recent 400 year uptrend

Modern observation

Main article: Solar observatory

The Swedish 1-m Solar Telescope at Roque de los Muchachos Observatory on La Palma in the Canary Islands

Sunspots are observed with land-based and Earth-orbiting solar telescopes. These telescopes use filtration and projection techniques for direct observation, in addition to various types of filtered cameras. Specialized tools such as spectroscopes and spectrohelioscopes are used to examine sunspots and sunspot areas. Artificial eclipses allow viewing of the circumference of the Sun as sunspots rotate through the horizon.

Since looking directly at the Sun with the naked eye permanently damages human vision, amateur observation of sunspots is generally conducted using projected images, or directly through protective filters. Small sections of very dark filter glass, such as a #14 welder's glass, are effective. A telescope eyepiece can project the image, without filtration, onto a white screen where it can be viewed indirectly, and even traced, to follow sunspot evolution. Special purpose hydrogen-alpha narrow bandpass filters and aluminum-coated glass attenuation filters (which have the appearance of mirrors due to their extremely high optical density) on the front of a telescope provide safe observation through the eyepiece.

Application

Due to their correlation with other kinds of solar activity, sunspots can be used to help predict space weather, the state of the ionosphere, and conditions relevant to short-wave radio propagation or satellite communications. High sunspot activity is celebrated by members of the amateur radio community as a harbinger of excellent ionospheric propagation conditions that greatly increase radio range in the HF bands. During peaks in sunspot activity, worldwide radio communication can be achieved on frequencies as high as the 6-meter VHF band.

Solar activity (and the solar cycle) have been implicated as a factor in global warming. The first possible example of this is the Maunder Minimum period of low sunspot activity which occurred during the Little Ice Age in Europe. However, detailed studies from multiple paleoclimate indicators show that the lower northern hemisphere temperatures in the Little Ice Age began while sunspot numbers were still high before the start of the Maunder Minimum, and persisted until after the Maunder Minimum had ceased. Numerical climate modelling indicates that volcanic activity was the main driver of the Little Ice Age.

Sunspots themselves, in terms of the magnitude of their radiant-energy deficit, have a weak effect on solar flux. The total effect of sunspots and other magnetic processes in the solar photosphere is an increase of roughly 0.1% in brightness of the Sun in comparison with its brightness at the solar-minimum level. This is a difference in total solar irradiance at Earth over the sunspot cycle of close to $1.37\ \mathrm {W\cdot m^{-1}}$. Other magnetic phenomena which correlate with sunspot activity include faculae and the chromospheric network. The combination of these magnetic factors mean that the relationship of sunspot numbers to Total Solar Irradiance (TSI) over the decadal-scale solar cycle. and their relationship for century timescales, need not be the same. The main problem with quantifying the longer-term trends in TSI lies in the stability of the absolute radiometry measurements made from space, which has improved in recent decades but remains a problem. Analysis shows that it is possible that TSI was actually higher in the Maunder Minimum compared to present-day levels, but uncertainties are high, with best estimates in the range $\pm 0.5\ \mathrm {W\cdot m^{-1}}$ with a $2\sigma$ uncertainty range of $\pm 1\ \mathrm {W\cdot m^{-1}}$.

Starspot

Main article: Starspot

In 1947, G. E. Kron proposed that starspots were the reason for periodic changes in brightness on red dwarfs. Since the mid-1990s, starspot observations have been made using increasingly powerful techniques yielding more and more detail: photometry showed starspot growth and decay and showed cyclic behavior similar to the Sun's; spectroscopy examined the structure of starspot regions by analyzing variations in spectral line splitting due to the Zeeman effect; Doppler imaging showed differential rotation of spots for several stars and distributions different from the Sun's; spectral line analysis measured the temperature range of spots and the stellar surfaces. For example, in 1999, Strassmeier reported the largest cool starspot ever seen rotating the giant K0 star XX Triangulum (HD 12545) with a temperature of 3,500 K (3,230 °C), together with a warm spot of 4,800 K (4,530 °C).

See also

• Letters on Sunspots
• Joy's law
• List of solar cycles
• Radio propagation
• Solar cycle
• Solar rotation
• Space weather
• Spörer's law (predictive)
• Starspot
• Wolf number sunspot number

Further reading

• Carl Luetzelschwab, K9LA (October 2016). "The new sunspot numbers". QST. 100 (10): 38–41. ISSN 0033-4812.

External links

• Sunspot Database based on Terrestrial (GPR/DPD) and Satellite (SOHO/SDO) observations from 1872 to Nowadays with the newest data. ()
• Solar Cycle 24 and VHF Aurora Website (www.solarcycle24.com)
• Belgium World Data Center for the sunspot index
• High resolution sunspot image
• Sunspot images in high-res Impressive collection of sunspot images
• NOAA Solar Cycle Progression: Current solar cycle.
  • Current conditions: Space weather
• Lockheed Martin Solar and Astrophysics Lab
• Sun|trek website An educational resource for teachers and students about the Sun and its effect on the Earth
• Tools to display the current sunspot number in a browser
  • Propfire – displays current sunspot number in browser status bar
  • HamLinks Toolbar – displays solar flux, A Index and K Index data in a toolbar
• The Sharpest View of the Sun
• Daily Sunspot Update and Picture of the Sun (www.spaceweather.com)
• Animated explanation of Sunspots in the Photosphere Archived 16 November 2015 at the Wayback Machine (University of South Wales)

Sunspot data

• "11,000 Year Sunspot Number Reconstruction". Global Change Master Directory. Archived from the original on 2 November 2015. Retrieved 11 March 2005.
  • "Unusual activity of the Sun during recent decades compared with the previous 11,000 years". WDC for Paleoclimatology. Retrieved 11 March 2005.
• "Sunspot Numbers from Ancient Times to Present from NOAA/NGDC". Global Change Master Directory. Archived from the original on 14 September 2015. Retrieved 11 March 2005.
  • "Sunspot Numbers". NOAA NGDC Solar Data Services. Retrieved 21 June 2010.
    • International Sunspot Number – sunspot maximum and minimum 1610–present; annual numbers 1700–present; monthly numbers 1749–present; daily values 1818–present; and sunspot numbers by north and south hemisphere. The McNish–Lincoln sunspot prediction is also included.
    • American sunspot numbers 1945–present
    • Ancient sunspot data 165 BC to 1684 AD
    • Group Sunspot Numbers (Doug Hoyt re-evaluation) 1610–1995
• Wilson, Robert M. (April 2014). Comparison of the Variations of Sunspot Number, Number of Sunspot Groups, and Sunspot Area, 1875-2013. Huntsville, AL: National Aeronautics and Space Administration, Marshall Space Flight Center. Retrieved 13 March 2015.