Observations of the eclipsing binary pulsar in Terzan 5

Journal Article · Mon Oct 01 00:00:00 EDT 1990 · Astrophysical Journal; (USA)

DOI:https://doi.org/10.1086/185827· OSTI ID:6174859

Nice, D J; Thorsett, S E; Taylor, J H; Fruchter, A S ^[1]

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1. Princeton Univ., NJ (USA) Carnegie Institution of Washington, Washington, DC (USA)

The eclipsing msec binary pulsar PSR 1744 - 24A was observed at radio frequencies between 800 MHz and 1.66 GHz. It is found that the pulsar is eclipsed behind its 0.1-solar-mass companion for up to half of each 109-min orbit, indicating that the companion's eclipsing region is much larger than its Roche lobe. Eclipse duration varies with observing frequency as nu exp beta, with beta = -0.63 + or - 0.18. The pulsed signal is weaker near eclipse boundaries, but no other changes in the pulses are observed. The signal sometimes disappears entirely for intervals as long as several hours. Delayed pulse arrival times after some such anomalous disappearances may suggest that they are caused by excess material in the vicinity of the binary system. 13 refs.

• OSTI ID: 6174859
• Journal Information: Astrophysical Journal; (USA), Journal Name: Astrophysical Journal; (USA) Vol. 361; ISSN ASJOA; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
BINARY STARS
COSMIC RADIO SOURCES
ECLIPSE
ELECTROMAGNETIC RADIATION
MASS
PULSARS
PULSES
RADIATIONS
RADIOWAVE RADIATION
ROCHE EQUIPOTENTIALS
STAR EVOLUTION
STARS