Abstract
With the recent detection of radio emission from dwarf novae a new channel of information on these semi-detached binaries has opened. The radiation is variable within days and highly polarized. Most likely it is emitted by some gyromagnetic process, which would allow to estimate the magnetic field. If it is synchrotron emission, the magnetic field strength in the source is of the order of 40 G; if interpreted by the cyclotron maser process the magnetic field is 800 – 1800 G depending on which harmonic of the local gyrofrequency is emitted. The radio emission seems to be limited to the later part of the optically high state of the accretion disk. This suggests an acceleration mechanism connected to the outburst.
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© 1989 Kluwer Academic Publishers
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Benz, A.O. (1989). Radio Emission of Dwarf Novae. In: Belvedere, G. (eds) Accretion Disks and Magnetic Fields in Astrophysics. Astrophysics and Space Science Library, vol 156. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-2401-7_12
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DOI: https://doi.org/10.1007/978-94-009-2401-7_12
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