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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/8831
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dc.contributor.authorRamesh, R-
dc.contributor.authorPriyal, M-
dc.contributor.authorSingh, J-
dc.contributor.authorSasikumar Raja, K-
dc.date.accessioned2025-12-31T08:56:53Z-
dc.date.available2025-12-31T08:56:53Z-
dc.date.issued2025-11-
dc.identifier.citationSolar Physics, Vol. 300, No. 11, 165en_US
dc.identifier.issn0038-0938-
dc.identifier.urihttp://hdl.handle.net/2248/8831-
dc.descriptionRestricted Accessen_US
dc.descriptionThe original publication is available at springerlink.com-
dc.description.abstractWe report long duration observations of changes in the 5303 Å (Fe XIV) solar coronal emission line parameters at heliocentric distance r≈1.07R⊙, using data obtained with the Visible Line Emission Coronagraph (VELC) onboard Aditya-L1 in the sit and stare mode. The observed changes are due to a flare near the east limb of the Sun. The intensity and width of the line are enhanced during the event. There is no change in the Doppler velocity. Our analysis indicates that the increase in line width is most likely due to an increase in temperature due to flare heatingen_US
dc.language.isoenen_US
dc.publisherSpringer Natureen_US
dc.relation.urihttps://doi.org/10.1007/s11207-025-02581-2-
dc.rights© The Author(s), under exclusive licence to Springer Nature B.V. 2025-
dc.subjectSun, activityen_US
dc.subjectSun, coronaen_US
dc.subjectSun, flaresen_US
dc.subjectSun, coronal mass ejectionsen_US
dc.subjectSun, spectroscopyen_US
dc.titleSpectroscopic observations of temporal changes in the 5303 Å solar coronal emission line during a flareen_US
dc.typeArticleen_US
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