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

Kundu, M. R.; Shevgaonkar, R. K.

doi:10.1007/978-94-009-5420-5_31

M. R. Kundu³ &
R. K. Shevgaonkar³

Part of the book series: Astrophysics and Space Science Library ((ASSL,volume 116))

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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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Authors and Affiliations

Astronomy Program, University of Maryland, College Park, MD, 20742, USA
M. R. Kundu & R. K. Shevgaonkar

Authors

M. R. Kundu
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R. K. Shevgaonkar
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Editors and Affiliations

National Radio Astronomy Observatory, Socorro, New Mexico, USA
Robert M. Hjellming
New Mexico Institute of Mining and Technology, Socorro, New Mexico, USA
David M. Gibson

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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
Print ISBN: 978-94-010-8892-3
Online ISBN: 978-94-009-5420-5
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