Astron. Astrophys. 351, 551-553 (1999)

Research Note

The peak radio emission phase variations in the Be-star/X-ray source LSI+61^o303

Krishna M.V. Apparao

Department of Physics, University of Bombay, Bombay 400098, India

Received 23 March 1999 / Accepted 1 September 1999

Abstract

The orbital phase of the peak radio emission in the Be star/X-ray source LSI +61^o 303 shows variations ranging from 0.5 to 0.9, the weaker emissions showing the larger phase. The delay in attaining peak emission is explained as due to the time required for the relativistic gas bubble responsible for the radio emission, expanding in the hot wind of the Be star, to become large enough in size to become optically thin at the radio frequencies.

Key words: accretion, accretion disks stars: binaries: general stars: emission-line, Be stars: individual: LSI +61O 303 radio continuum: stars X-rays: stars

SIMBAD Objects

Contents

• 1. Introduction
• 2. Escape of the plasmon from the cool disk of the Be star
• 3. Expansion of the plasmon
• 4. Discussion
• Acknowledgements
• References

© European Southern Observatory (ESO) 1999

Online publication: November 3, 1999
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