Microwave emission from late-type dwarf stars UV Ceti and YZ Canis Minoris

Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/5239

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DC Field	Value	Language
dc.contributor.author	Kundu, M. R	-
dc.contributor.author	Shevgaonkar, R. K	-
dc.date.accessioned	2010-09-01T12:31:17Z	-
dc.date.available	2010-09-01T12:31:17Z	-
dc.date.issued	1985-10-15	-
dc.identifier.citation	The Astrophysical Journal, Vol. 297, pp. 644 - 648	en
dc.identifier.uri	http://hdl.handle.net/2248/5239	-
dc.description	Open Access	en
dc.description.abstract	Simultaneous high-resolution observations of two late-type dwarf stars, UV Cet and YZ CMi, at 6 and 20 cm are presented. These observations put sufficient constraints on existing interpretations to conclude that the quiescent microwave emission from these stars is due to gyrosynchrotron radiation of nonthermal electrons having a power-law energy distribution. From the lifetime of 1 hr of the nonthermal particles against radiation and collision losses, a magnetic field of a few thousand gauss on the photosphere of these stars is estimated. The observations indicate that the ambient density in the coronae of YZ CMi is an order of magnitude higher than that of UV Cet.	en
dc.language.iso	en	en
dc.publisher	The University of Chicago Press	en
dc.relation.uri	http://adsabs.harvard.edu/abs/1985ApJ...297..644K	en
dc.rights	© The American Astronomical Society	en
dc.subject	Radiation Mechanisms	en
dc.subject	Stars-Individual	en
dc.subject	Stars: Late-Type	en
dc.subject	Stars: Radio Radiation	en
dc.title	Microwave emission from late-type dwarf stars UV Ceti and YZ Canis Minoris	en
dc.type	Article	en
Appears in Collections:	IIAP Publications

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