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

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

Oct 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...297..644k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 297, Oct. 15, 1985, p. 644-648.

Astronomy and Astrophysics

Astrophysics

33

Dwarf Stars, Flare Stars, Late Stars, Microwave Emission, Stellar Radiation, Astronomical Maps, Circular Polarization, Nonthermal Radiation, Particle Collisions, Photosphere, Stellar Magnetic Fields, Synchrotron Radiation

Scientific paper

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.

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