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Title:
The Unusual Binary Pulsar PSR J1744-3922: Radio Flux Variability, Near-Infrared Observation, and Evolution
Authors:
Breton, R. P.; Roberts, M. S. E.; Ransom, S. M.; Kaspi, V. M.; Durant, M.; Bergeron, P.; Faulkner, A. J.
Affiliation:
AA(Department of Physics, McGill University, Montreal, QC H3A 2T8, Canada; .), AB(Eureka Scientific, Inc., Oakland, CA 94602-3017.), AC(National Radio Astronomy Observatory, Charlottesville, VA 22903.), AD(Department of Physics, McGill University, Montreal, QC H3A 2T8, Canada; .), AE(Department of Astronomy and Astrophysics, University of Toronto, Toronto, ON M5S 3H8, Canada.), AF(Département de Physique, Université de Montréal, Montréal, QC H3C 3J7, Canada.), AG(University of Manchester, Jodrell Bank Observatory, Macclesfield, Cheshire, SK11 9DL, UK.)
Publication:
The Astrophysical Journal, Volume 661, Issue 2, pp. 1073-1083. (ApJ Homepage)
Publication Date:
06/2007
Origin:
UCP
ApJ Keywords:
pulsars: individual (PSR J1744-3922), Stars: Evolution
DOI:
10.1086/515392
Bibliographic Code:
2007ApJ...661.1073B

Abstract

PSR J1744-3922 is a binary pulsar exhibiting highly variable pulsed radio emission. We report on a statistical multifrequency study of the pulsed radio flux variability which suggests that this phenomenon is extrinsic to the pulsar and possibly tied to the companion, although not strongly correlated with orbital phase. The pulsar has an unusual combination of characteristics compared to typical recycled pulsars: a long spin period (172 ms); a relatively high magnetic field strength (1.7×1010 G); a very circular, compact orbit of 4.6 hr; and a low-mass companion (0.08 Msolar). These spin and orbital properties are likely inconsistent with standard evolutionary models. We find similarities between the properties of the PSR J1744-3922 system and those of several other known binary pulsar systems, motivating the identification of a new class of binary pulsars. We suggest that this new class could result from: a standard accretion scenario of a magnetar or a high magnetic field pulsar; common envelope evolution with a low-mass star and a neutron star, similar to what is expected for ultracompact X-ray binaries; or accretion induced collapse of a white dwarf. We also report the detection of a possible K'=19.30(15) infrared counterpart at the position of the pulsar, which is relatively bright if the companion is a helium white dwarf at the nominal distance, and discuss its implications for the pulsar's companion and evolutionary history.
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