Circular Polarization Observations of Type II Solar Radio Bursts and the Coronal Magnetic Field

Ramesh, R; Kathiravan, C; Ebenezer, E

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dc.contributor.author	Ramesh, R
dc.contributor.author	Kathiravan, C
dc.contributor.author	Ebenezer, E
dc.date.accessioned	2022-08-24T05:48:10Z
dc.date.available	2022-08-24T05:48:10Z
dc.date.issued	2022-06-10
dc.identifier.citation	The Astrophysical Journal, Vol. 932, No. 1, 48	en_US
dc.identifier.issn	1538-4357
dc.identifier.uri	http://hdl.handle.net/2248/8026
dc.description	Open Access	en_US
dc.description	Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.
dc.description.abstract	It is well known that magnetic field strength (B) in the solar corona can be calculated using the Alfvén Mach number (MA) and Alfvén speed (vA) of the magnetohydrodynamic shock waves associated with coronal type II radio bursts. We show that observations of weak circularly polarized emission associated with the harmonic component of the type II bursts provide independent and consistent estimates of B. For the coronal type II burst observed on 2021 October 9, we obtained B ≈1.5 G and ≈1.9 G at a heliocentric distance (r) of ≈1.8 Re, using the above two techniques, respectively.	en_US
dc.language.iso	en	en_US
dc.publisher	American Astronomical Society	en_US
dc.relation.uri	https://doi.org/10.3847/1538-4357/ac6f05
dc.rights	© 2022 The Author(s)
dc.subject	Solar coronal mass ejections	en_US
dc.subject	The Sun	en_US
dc.subject	Solar magnetic fields	en_US
dc.subject	Solar radio emission	en_US
dc.subject	Solar corona	en_US
dc.title	Circular Polarization Observations of Type II Solar Radio Bursts and the Coronal Magnetic Field	en_US
dc.type	Article	en_US