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New Evidence for a Coronal Mass Ejection-driven High Frequency Type II Burst near the Sun

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dc.contributor.author Anshu Kumari
dc.contributor.author Ramesh, R
dc.contributor.author Kathiravan, C
dc.contributor.author Gopalswamy, N
dc.date.accessioned 2020-11-10T01:47:37Z
dc.date.available 2020-11-10T01:47:37Z
dc.date.issued 2017-07
dc.identifier.citation The Astrophysical Journal, Vol. 843, No. 1, 10 en_US
dc.identifier.issn 0004-637X
dc.identifier.uri http://prints.iiap.res.in/handle/2248/6688
dc.description restricted Access © The American Astronomical Society https://doi.org/10.3847/1538-4357/aa72e7 en_US
dc.description.abstract We report observations of the high frequency type II radio burst (≈430–30 MHz) that occurred in the solar corona on 2015 November 4. The drift rate of the burst, estimated close to the start frequency of its fundamental component (≈215 MHz), is unusually high (≈2 MHz s−1 ). Our analysis shows that the estimated speed of the magnetohydrodynamic shock driver of the burst varies with time. The peak speed and acceleration are very large, » - 2450 km s 1 and » - 17 km s 2, respectively. There is spatio-temporal correlation between the type II burst and the associated coronal mass ejection (CME) in the whitelight and extreme-ultraviolet images. The time profile of the shock speed and the light curve of the associated soft X-ray flare correlate well. These results indicate that in the present case, (i) the magnetohydrodynamic shock responsible for the high frequency coronal type II burst is driven by the CME and (ii) the time profile of the type II burst shock speed represents the near-Sun kinematics of the CME en_US
dc.language.iso en en_US
dc.publisher IOP Publishing en_US
dc.subject Sun: activity en_US
dc.subject Sun: corona en_US
dc.subject coronal mass ejections (CMEs) en_US
dc.subject Sun: flares en_US
dc.subject Sun: magnetic fields en_US
dc.subject radio radiation en_US
dc.title New Evidence for a Coronal Mass Ejection-driven High Frequency Type II Burst near the Sun en_US
dc.type Article en_US


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