Sunspot groups
The sunspot number is calculated by first counting the number of sunspot groups and then the number of individual sunspots.
Sunspot Group Classification. (Modified Zurich Sunspot Classification). A - A small single unipolar sunspot or very small group of spots without penumbra. B - Bipolar sunspot group with no penumbra. C - An elongated bipolar sunspot group.
Sunspot Group - A cluster of sunspots
Supergiant - An extremely luminous star of large size and mass
Supergranulation - The pattern of very large (15,000 to 30,000 km in diameter) convective cells in the Sun's photosphere ...
Sunspot Group
This image of the whole solar disk shows the sunspot group size of the images. The diameter of the Sun is 100 times larger than the diameter of the Earth.
Sunspot group 9393
Christmas 2000 partial eclipse sequence of images
Christmas 2000 partial eclipse time lapse video (422KB requires media player)
Moon
Images with 8 inch f/10 LX200 ...
B-Bipolar sunspot group with no penumbra.
C-An elongated bipolar sunspot group. One sunspot must have penumbra, and penumbra does not exceed 5 ° in longitudinal extent.
Closeup large sunspot group as seen through my 10-inch Meade Schmidt Cassegrain telescope in Orlando, Florida on 3/14/89. This image was captured on Kodak Ektachrome 100 color slide film with a Thousand Oaks full-aperture glass solar filter.
LEADER SPOT In a magnetically bipolar or multipolar SUNSPOT group, the western part precedes and the main spot in that part is called the leader.
Faculae are slightly brighter areas that form around sunspot groups as the flow of energy to the photosphere is re-established and both the normal flow and the sunspot-blocked energy elevate the radiating 'surface' temperature.
All the major activity events are linked with sunspots - prominences tend to erupt from sunspot groups, CMEs come from sunspot groups, and flares come from the areas of sunspot groups. I am noticing a trend here.
A solar flare is a sudden intense brightening of a small part of the Sun's chromosphere in the vicinity of a plage or facula and often near a sunspot group. The flare develops in a few minutes and may last several hours.
Large sunspot groups moving across the sun's equator temporarily decrease the flux. This occurred April 3-10, 1980 when the Solar Maximum Mission on Nimbus 7 revealed a decrease of about 1.
Since most sunspot groups have, on average, about ten spots, this formula for counting sunspots gives reliable numbers even when the observing conditions are less than ideal and small spots are hard to see.
Solar activity tends to be concentrated in active regions associated with sunspot groups. Prominences are loop- or sheetlike structures produced when hot gas ejected by activity on the solar surface interacts with the Sun's magnetic field.
sunspot groups) cancel each other, creating "neutral points" of zero field intensity. Such points--unfortunately for experimenters--are usually well above the photosphere, in region whose magnetic fields are difficult to measure.
The "sunspot number" (SSN) is calculated by counting he number of sunspot groups, then the number of individual spots, and the SSN is given as the sum of the number of individual spots plus ten times the number of groups.
where k is a factor that attempts to account for the other variables in the measurement. Note that typical sunspot groups contain about 10 spots on average.
Sudden brightening of a region of the Sun's surface, almost invariably within or near complex sunspot groups.
FLARE STAR ...
R = k (10g + f) where k is a constant depending on observing conditions, g is the number of sunspot groups, and f is the number of individual spots visible on the Sun at a given time. [H76]
Wolf-Rayet (WR) Star ...
(Also called the Relative Number) A quantity which gives the number of sunspots, and the number of groups of sunspots, at a given time. R = k (10g + f) where k is a constant depending on observing conditions, g is the number of sunspot groups, ...
In one 11-year cycle the leading sunspot in a sunspot group will have a north magnetic pole while the trailing sunspot in the group will have a south magnetic pole. In the next 11-year cycle the poles will switch so the total cycle is 22 years long.
Afterwards, students are given several time-sequenced images of a region with a growing sunspot group in white light and H-alpha, and are challenged to put them in time order.
Most solar flares and coronal mass ejections originate in magnetically active regions around sunspot groupings. Similar phenomena observed on stars other than the Sun are commonly called starspots.
Sunspot variation ...
 See also: Solar, Sunspot, Field, Sun, Sunspots
  
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