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Quasi-periodic oscillation of a coronal bright point

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dc.contributor.author Samanta, T
dc.contributor.author Banerjee, D
dc.contributor.author Tian, H
dc.date.accessioned 2020-11-12T14:50:09Z
dc.date.available 2020-11-12T14:50:09Z
dc.date.issued 2015-06-20
dc.identifier.citation The Astrophysical Journal, Vol. 806, No. 2, 172 en_US
dc.identifier.issn 0004-637X
dc.identifier.uri http://prints.iiap.res.in/handle/2248/6936
dc.description Restricted Access © IOP Publishing http://dx.doi.org/10.1088/0004-637X/806/2/172 en_US
dc.description.abstract Coronal bright points (BPs) are small-scale luminous features seen in the solar corona. Quasi-periodic brightenings are frequently observed in the BPs and are generally linked with underlying magnetic flux changes. We study the dynamics of a BP seen in the coronal hole using the Atmospheric Imaging Assembly images, the Helioseismic and Magnetic Imager magnetogram on board the Solar Dynamics Observatory, and spectroscopic data from the newly launched Interface Region Imaging Spectrograph (IRIS). The detailed analysis shows that the BP evolves throughout our observing period along with changes in underlying photospheric magnetic flux and shows periodic brightenings in different EUV and far-UV images. With the highest possible spectral and spatial resolution of IRIS, we attempted to identify the sources of these oscillations. IRIS sit-and-stare observation provided a unique opportunity to study the time evolution of one footpoint of the BP as the slit position crossed it. We noticed enhanced line profile asymmetry, enhanced line width, intensity enhancements, and large deviation from the average Doppler shift in the line profiles at specific instances, which indicate the presence of sudden flows along the line-of-sight direction. We propose that transition region explosive events originating from small-scale reconnections and the reconnection outflows are affecting the line profiles. The correlation between all these parameters is consistent with the repetitive reconnection scenario and could explain the quasi-periodic nature of the brightening. en_US
dc.language.iso en en_US
dc.publisher IOP Publishing en_US
dc.subject Sun: corona en_US
dc.subject Sun: magnetic fields en_US
dc.subject Sun: oscillations en_US
dc.subject Sun: transition region en_US
dc.subject Sun: UV radiation en_US
dc.title Quasi-periodic oscillation of a coronal bright point en_US
dc.type Article en_US


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