dc.contributor.author |
Suryanarayana, G. S |
|
dc.date.accessioned |
2020-11-11T01:37:56Z |
|
dc.date.available |
2020-11-11T01:37:56Z |
|
dc.date.issued |
2018-03 |
|
dc.identifier.citation |
Research in Astronomy and Astrophysics, Vol. 18, No. 3, 34 |
en_US |
dc.identifier.issn |
1674-4527 |
|
dc.identifier.uri |
http://prints.iiap.res.in/handle/2248/6878 |
|
dc.description |
Restricted Access © National Astronomical Observatories, CAS and IOP Publishing Ltd.; https://doi.org/10.1088/1674-4527/18/3/34 |
en_US |
dc.description.abstract |
Flare characteristics such as the flare occurrence number density and the distribution of peak flux as well as duration of flares occurring on either side of a coronal mass ejection (CME) onset time are studied. While the flares are rather evenly distributed statistically on either side of the CME onset time, the flare peak flux and duration tend to decrease depending upon their occurrence either before or after the CME onset. This is consistent with the earlier findings that flares emit higher energy before a CME whereas the energy is less in flares occurring after a CME. |
en_US |
dc.language.iso |
en |
en_US |
dc.publisher |
IOP Publishing |
en_US |
dc.subject |
Sun: flares |
en_US |
dc.subject |
Sun: coronal mass ejections |
en_US |
dc.subject |
Sun: peak flux of flares |
en_US |
dc.subject |
Sun: flare durations |
en_US |
dc.title |
Flares before and after coronal mass ejections |
en_US |
dc.type |
Article |
en_US |