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Strength of the Solar Coronal Magnetic Field A Comparison of Independent Estimates Using Contemporaneous Radio and White-Light Observations

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dc.contributor.author Anshu Kumari
dc.contributor.author Ramesh, R
dc.contributor.author Kathiravan, C
dc.contributor.author Wang, T. J
dc.date.accessioned 2020-11-12T15:13:54Z
dc.date.available 2020-11-12T15:13:54Z
dc.date.issued 2017-11
dc.identifier.citation Solar Physics, Vol. 292, No. 11, 161 en_US
dc.identifier.issn 0250-6335
dc.identifier.uri http://prints.iiap.res.in/handle/2248/6969
dc.description Restricted Access © Springer The original publication is available at springerlink.com https://doi.org/10.1007/s11207-017-1180-6 en_US
dc.description.abstract Abstract We estimated the coronal magnetic field strength (B) during the 23 July 2016 coronal mass ejection (CME) event using i) the flux rope structure of the CME in the whitelight coronagraph images and ii) the band-splitting in the associated type II burst. No models were assumed for the coronal electron density (N(r)) we used in the estimation. The results obtained with these two independent methods correspond to different heliocentric distances (r) in the range ≈ 2.5 – 4.5 R , but they show excellent consistency and could be fit with a single power-law distribution of the type B(r) = 5.7r−2.6 G, which is applicable in that distance range. The power-law index (i.e. −2.6) is in good agreement with the results obtained in previous studies by different methods. en_US
dc.language.iso en en_US
dc.publisher Springer en_US
dc.subject Sun en_US
dc.subject Coronal mass ejections en_US
dc.subject Radio bursts en_US
dc.subject Coronal magnetic field en_US
dc.title Strength of the Solar Coronal Magnetic Field A Comparison of Independent Estimates Using Contemporaneous Radio and White-Light Observations en_US
dc.type Article en_US


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