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Transient radio emission from PSR B1259–63

Published online by Cambridge University Press:  12 April 2016

Lewis Ball ,
Andrew Melatos ,
Simon Johnston  and
Olaf Skjæraasen
Lewis Ball
Affiliation:
Research Centre for Theoretical Astrophysics, Univ. Sydney, Australia
Andrew Melatos
Affiliation:
Miller Fellow, Dept. of Astronomy, Univ. California, Berkeley, USA
Simon Johnston
Affiliation:
Research Centre for Theoretical Astrophysics, Univ. Sydney, Australia
Olaf Skjæraasen
Affiliation:
Research Centre for Theoretical Astrophysics, Univ. Sydney, Australia Institute of Theoretical Astrophysics, Univ. Oslo, Norway

Abstract

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The unique binary pulsar system PSR B1259–63, comprising a radio pulsar in an eccentric orbit about a hot, massive companion star, has been extensively monitored at radio frequencies between 843 MHz and 8.4 GHz during its 1994 and 1997 periastron passages. Unpulsed radio emission was detected for about 100 days around each periastron, varying on time scales as short as a day. We argue that the emission is synchrotron radiation generated as the pulsar passes through the Be-star’s excretion disk just before and just after periastron.

Type
Part 7. The Surrounding of Pulsars
Information
International Astronomical Union Colloquium , Volume 177: Pulsar Astronomy - 2000 and Beyond , 2000 , pp. 529 - 530
Copyright
Copyright © Astronomical Society of the Pacific 2000

References

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