Abstract
We 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. We find 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. From the lifetime of several hours of the nonthermal particles against radiation and collisional losses we estimate a magnetic field of ~ 140 G and a density of ≲ 2 × 10 cm-3 in the microwave source.
On leave of Absence from Indian Institute of Astrophysics, Bangalore, India
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© 1985 D. Reidel Publishing Company
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Kundu, M.R., Shevgaonkar, R.K. (1985). Microwave Emission from Late Type Dwarf Stars UV Ceti and YZ CMi. In: Hjellming, R.M., Gibson, D.M. (eds) Radio Stars. Astrophysics and Space Science Library, vol 116. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-5420-5_31
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DOI: https://doi.org/10.1007/978-94-009-5420-5_31
Publisher Name: Springer, Dordrecht
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