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Rotational and Orbital Fluctuations of Eclipsing Binary Pulsar PSR B1744-24A
Published online by Cambridge University Press: 12 April 2016
Extract
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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