Sunspots form on the surface of the Sun due to strong magnetic field lines coming up from within the Sun trough the solar surface and appear visibly as dark spots compared to their surroundings. These sunspots which can become many times bigger than the Earth are always dark because they are much cooler than the surrounding surface of the Sun itself. A big sunspot can have a temperature of 3700°C. This sounds like much but if we compare this with the temperature of the photosphere of the Sun which is about 5500°C, then you see that there is a considerable difference. As a matter of fact, if we could take a sunspot out of the Sun and place it into our night sky it would only be as bright as the full moon, a very big contrast with the bright Sun itself.
Sunspots are a common sight on our Sun during the years around solar maximum. Solar maximum or solar max is the period of greatest solar activity in the solar cycle of the Sun, where one solar cycle lasts about 11 years. Around solar minimum, only very few or even no sunspots can be found. Sunspots form where magnetic field lines come up from the Sun's interior trough the solar surface meaning that every sunspot has it's own polarity.
A sunspot consists of two parts:
The image below shows a large and complex group with numerous sunspots. This is called a sunspot group or an Active Region. Every day, all the sunspot groups on the Earth-facing solar disk are analysed for their eruptive threat and receive a number. This is done by the NOAA Space Weather Prediction Center. Groups of sunspots, especially those with complex magnetic layouts, are know to cause a phenomenon called solar flares.
The Sun rotates around its axis just like Earth does. Solar features on the Sun like sunspot regions follow the rotation of the Sun. This means that a sunspot region travels across the solar disk from east to west as seen from Earth. This is important because sunspot regions need to be close to the central meridian (as seen from Earth) in order to be able to send coronal mass ejection towards Earth. It takes a sunspot region near the equator about 2 weeks to move from the east limb to west limb as seen from Earth. The further away a sunspot region is from the equator the longer it takes move across the face of the Sun. This is because the Sun rotates faster at its equator than at its poles. The rotational period is approximately 25.6 days at the equator and 33.5 days at the poles. Viewed from Earth as it orbits the Sun, the apparent rotational period of the Sun at its equator is about 28 days.
Animation: Very large sunspot region 2192 rotates across the Earth-facing solar disk as seen by the Solar Dynamics Observatory.
|Wysokie szerokości geograficzne||20%||15%|
|Średnie szerokości geograficzne||5%||1%|
|Przewidywane Kp max||3|
|klasy M rozbłysk słoneczny||1%|
|klasy X rozbłysk słoneczny||1%|
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|Ostatnie rozbłyski klasy X:||2017/09/10||X8.2|
|Ostatnie rozbłyski klasy M:||2017/10/20||M1.0|
|Ostatnia burza geomagnetyczna:||2017/11/08||Kp6 (G2)|
|Ilość dni bez skazy w 2017 roku:||81|
|Ostatni dzień bez skazy:||2017/11/13|