dc.contributor.author |
Chatterjee, Piyali |
|
dc.contributor.author |
Hansteen, V |
|
dc.contributor.author |
Carlsson, M |
|
dc.date.accessioned |
2020-11-19T13:47:48Z |
|
dc.date.available |
2020-11-19T13:47:48Z |
|
dc.date.issued |
2016-03 |
|
dc.identifier.citation |
Physical Review Letters, Vol. 116, No.10, 101101 |
en_US |
dc.identifier.issn |
0031-9007 |
|
dc.identifier.uri |
http://prints.iiap.res.in/handle/2248/7260 |
|
dc.description |
Open Access © American Physical Society http://dx.doi.org/10.1103/PhysRevLett.116.101101 |
en_US |
dc.description.abstract |
Active regions (ARs) appearing on the surface of the Sun are classified into α , β , γ , and δ by the rules of the Mount Wilson Observatory, California on the basis of their topological complexity. Amongst these, the δ sunspots are known to be superactive and produce the most x-ray flares. Here, we present results from a simulation of the Sun by mimicking the upper layers and the corona, but starting at a more primitive stage than any earlier treatment. We find that this initial state consisting of only a thin subphotospheric magnetic sheet breaks into multiple flux tubes which evolve into a colliding-merging system of spots of opposite polarity upon surface emergence, similar to those often seen on the Sun. The simulation goes on to produce many exotic δ sunspot associated phenomena: repeated flaring in the range of typical solar flare energy release and ejective helical flux ropes with embedded cool-dense plasma filaments resembling solar coronal mass ejections. |
en_US |
dc.language.iso |
en |
en_US |
dc.publisher |
The American Physical Society |
en_US |
dc.subject |
Solar and Stellar Astrophysics |
en_US |
dc.title |
Modeling Repeatedly Flaring δ Sunspots |
en_US |
dc.type |
Article |
en_US |