Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/7267
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dc.contributor.authorSuryanarayana, G. S-
dc.date.accessioned2018-04-18T03:47:50Z-
dc.date.available2018-04-18T03:47:50Z-
dc.date.issued2018-03-
dc.identifier.citationResearch in Astronomy and Astrophysics, Vol. 18, No. 3, 34en_US
dc.identifier.issn1674-4527-
dc.identifier.urihttp://hdl.handle.net/2248/7267-
dc.descriptionRestricted Accessen_US
dc.description.abstractFlare 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.isoenen_US
dc.publisherIOP Publishingen_US
dc.relation.urihttps://doi.org/10.1088/1674-4527/18/3/34-
dc.subjectSun: flaresen_US
dc.subjectSun: flare durationsen_US
dc.subjectSun: peak flux of flaresen_US
dc.subjectSun: coronal mass ejectionsen_US
dc.titleFlares before and after coronal mass ejectionsen_US
dc.typeArticleen_US
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