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Periodic Radio Emission from the Helium Rich Stars HD 37017 and σ Ori E

Published online by Cambridge University Press:  12 April 2016

Francesco Leone  and
Grazia Umana
Francesco Leone
Affiliation:
Osservatorio Astrofisico di Catania, Città Universitaria, I-95125 CataniaItaly
Grazia Umana
Affiliation:
Istituto di Radio Astronomia del C.N.R., VLBI station, P.O. Box 169 Noto, Italy

Abstract

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Drake et al. (1987) detected, for the first time, radio emission from magnetic Chemically Peculiar stars. They suggested that radio emission is consistent with gyrosynchrotron emission from continuously injected, mildly, relativistic particles trapped in a magnetic equatorial belt.

Leone (1991) showed that it is possible considering that the radio emission comes from magnetic poles and is due to the electron component of the wind flowing along the open field lines. As a consequence Leone (1991) put forward the hypothesis that such emission could be periodically variable.

In order to verify the surmise of a periodic radio emission, the magnetic Chemically Peculiar stars HD 37017 and σ Ori E have been monitored with the VLA at 6 cm.

By combining our data with those obtained by Drake et al. (1987) and Philips & Lestrade (1988), we show that the radio emission from HD 37017 and σ Ori E varies with the rotational period.

Type
VI. Magneto-Hydrodynamical Phenomena in CP Stars
Information
International Astronomical Union Colloquium , Volume 138: Peculiar versus Normal Phenomena in A-Type and Related Stars , 1993 , pp. 541 - 546
Copyright
Copyright © Astronomical Society of the Pacific 1993

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