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Insolar physics and observation, an active region is a temporary feature in the Sun's atmosphere characterized by a strong and complex magnetic field. They are often associated with sunspots and are commonly the source of violent eruptions such as coronal mass ejections and solar flares.[1] The number and location of active regions on the solar disk at any given time is dependent on the solar cycle.[2][3][4][5][6]
Newly observed active regions on the solar disk are assigned 4-digit region numbers by the Space Weather Prediction Center (SWPC) on the day following the initial observation. The region number assigned to a particular active region is one added to the previously assigned number. For example, the first observation of active region 8090, or AR8090, was followed by AR8091.
According to the SWPC, a number is assigned to a region if it meets at least one of the following criteria:[7]
The region numbers reached 10,000 in July 2002. However, the SWPC continued using 4-digits, with the inclusion of leading zeros.[8][9]
The Mount Wilson magnetic classification system, also known as the Hale magnetic classification system, is a method of classifying the magnetic field of active regions. It was first introduced in 1919 by George Ellery Hale and coworkers working at the Mount Wilson Observatory.[10] It originally included only the α, β, and γ magnetic classifications, but it was later modified by H. Künzel in 1965 to include the δ qualifier.[11][9]
| Classification | Description[12][9][13] |
|---|---|
| α | An active region containing a single sunspot or group of sunspots all having the same magnetic polarity. An opposite polarity counterpart is still present, but is weak or not concentrated enough to form sunspots. |
| β | An active region with at least two sunspots or sunspot groups that have opposite magnetic polarity. A simple neutral line between the two polarities is also present. |
| γ | An active region with sunspots having completely intermixed magnetic polarity. |
| β-γ | An active region with at least two sunspots or sunspot groups that have opposite magnetic polarity (hence β) but no well-defined neutral line dividing the opposite polarities (hence γ). |
| δ | A qualifier to the other classes indicating the presence of opposite polarity umbrae within a single penumbra separated by at most 2° in heliographic distance. |
| β-δ | An active region with a β magnetic field and at least one pair of opposite polarity umbrae within a single penumbra (hence δ). |
| β-γ-δ | An active region with a β-γ magnetic field and at least one pair of opposite polarity umbrae within a single penumbra (hence δ). |
| γ-δ | An active region with a γ magnetic field and at least one pair of opposite polarity umbrae within a single penumbra (hence δ). |
The strong magnetic flux found in active regions is often strong enough to inhibit convection. Without convection transporting energy from the Sun's interior to the photosphere, surface temperature decreases along with the intensity of emitted black body radiation. These areas of cooler plasma are known as sunspots, and often appear in groups.[14] However, not all active regions possess sunspots.[8]
Active regions form through the process of magnetic flux emergence, during which magnetic fields generated by the solar dynamo emerge from the solar interior.[15][16][17]: 118
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