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Rotational and Orbital Fluctuations of Eclipsing Binary Pulsar PSR B1744-24A

Published online by Cambridge University Press:  12 April 2016

David J. Nice  and
Stephen E. Thorsett
David J. Nice
Affiliation:
National Radio Astronomy Observatory Edgemont Road, Charlottesville VA 22903, USA
Stephen E. Thorsett
Affiliation:
Physics Department, Princeton UniversityBox 708, Princeton NJ 08544, USA

Extract

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Eclipsing binary pulsars systems highlight an important stage in the evolution of isolated millisecond pulsars. In these systems, the pulsar’s companion is losing mass due to Roche lobe overflow and/or a stellar wind induced by intercepted energy from the pulsar flux. Eventual evaporation of the companions could yield isolated millisecond puslars. PSR B1744-24A was the second eclipsing millisecond pulsar to be discovered (Lyne et al. 1990). It is in a 1.8 hr orbit with a ∼ 0.1 M⊙ companion. Its eclipses show some variability, and the pulsar is undetectable at about 25% of observing epochs, presumably because it is completely enveloped by the companion’s outflow (Nice & Thorsett 1992).

Type
Part 7 Binary Systems
Information
International Astronomical Union Colloquium , Volume 160: Pulsars: Problems and Progress , 1996 , pp. 523 - 524
Copyright
Copyright © Astronomical Society of the Pacific 1996

References

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