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Flares before and after coronal mass ejections

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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


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