Microwave Emission from Late Type Dwarf Stars UV Ceti and YZ CMi

Details Microwave Emission from Late Type Dwarf Stars UV Ceti and YZ CMi Microwave Emission from Late Type Dwarf Stars UV Ceti and YZ CMi

Jul 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985assl..116..229k&link_type=abstract

Radio Stars, proceedings of a workshop on stellar continuum radio astronomy, held in Boulder, CO, 8-10 August, 1984. Edited by

Astronomy and Astrophysics

Astrophysics

Scientific paper

The authors present simultaneous VLA observations of two late type dwarf stars UV Ceti and YZ CMi at 6 and 20 cm. Multiwavelength observations put sufficient constraints on existing interpretations of quiescent radio emission from these stars. They found that the microwave emission is due to gyro-synchrotron radiation of nonthermal electrons having a power law energy distribution. This emission originates from a source whose size is 2 - 3 times larger than the star. The authors estimate a magnetic field of ≡140 G and a density of ⪉2×108cm-3 in the microwave source.

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