Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996pasj...48..833h&link_type=abstract
Publications of the Astronomical Society of Japan, v.48, p.833-840.
Astronomy and Astrophysics
Astronomy
26
Pulsars, Stars: Be, Stars: Individual (Psr B1259-63), Stars: Individual (Ss 2883), X-Rays: Binaries
Scientific paper
We report on the results of a post-periastron ASCA observation of the PSR B1259-63 system, containing a 48 ms pulsar orbiting a Be star in an eccentric 3.4 yr orbit. The ASCA observation was carried out on 1994 February 28 when the radio pulsar was again visible after a prolonged 40-day radio eclipse near to periastron. The source was clearly detected with an X-ray luminosity (1--10 keV) L_X of ( 1.03 +/- 0.09 ) times 10(34) \ (d/2 kpc)(2) erg s(-1) , where d is the pulsar's distance. The X-ray spectrum is well-represented by a single power-law model of the photon index, alpha = 1.61 +/- 0.06, and a small photoelectric absorption, N_H = (5.6 +/- 0.6) times 10(21) cm(-2) . No significant X-ray pulsations were detected, and the upper limit for the pulsed component was estimated to be 15% of the total X-ray flux, assuming sinusoidal modulation. The characteristics of the X-ray emission detected on 1994 February 28 are similar to those detected by ASCA near periastron when the pulsed radio emission from PSR B1259-63 was eclipsed. Our results strongly favor a non-thermal model of X-ray emission driven by synchrotron radiation from relativistic shocked particles in the pulsar wind interacting with the outflow from the Be star companion.
Arons Jonathan
Hirayama Masaharu
Kaspi Victoria M.
Kawai Nobuyuki
Nagase Fumiaki
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