Origin of the transient unpulsed radio emission from the PSR B1259-63 binary system

Abstract

We discuss the interpretation of transient, unpulsed radio emission detected from the unique pulsar/Be-star binary system PSR B1259-63. Extensive monitoring of the 1994 and 1997 periastron passages has shown that the source flares over a 100-day interval around periastron, varying on time-scales as short as a day and peaking at 60 mJy (~100 times the apastron flux density) at 1.4 GHz. Interpreting the emission as synchrotron radiation, we show that (i) the observed variations in flux density are too large to be caused by the shock interaction between the pulsar wind and an isotropic, radiatively driven, Be-star wind, and (ii) the radio emitting electrons do not originate from the pulsar wind. We argue instead that the radio electrons originate from the circumstellar disk of the Be star and are accelerated at two epochs, one before and one after periastron, when the pulsar passes through the disk. A simple model incorporating two epochs of impulsive acceleration followed by synchrotron cooling reproduces the essential features of the radio light curve and spectrum and is consistent with the system geometry inferred from pulsed radio data.

arXiv commentTo be published in Astrophysical Journal Letters 7 pages, 1 postscript figure

References in corpus (3)

• Theory of high-energy emission from the pulsar/Be-star system PSR 1259$-$63 I: radiation mechanisms and interaction geometry
• Inverse Compton Emission of TeV Gamma Rays from PSR B1259-63
• Timing models for the long-orbital period binary pulsar PSR B1259-63

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