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

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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


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