ASCA Observations of the Unusual Binary LSI+61 Deg 303

Details ASCA Observations of the Unusual Binary LSI+61 Deg 303 ASCA Observations of the Unusual Binary LSI+61 Deg 303

Jan 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996cit..reptr....h&link_type=abstract

Technical Report, California Inst. of Tech. Pasadena, CA United States Space Radiation Lab.

Computer Science

X Rays, Radio Observation, Binary Stars, Radio Frequencies, Frequencies, Interferometers, Large Scale Integration, Neutron Stars, Pulsars, Radiant Flux Density, Shock Wave Interaction, Unsteady Flow

Scientific paper

We present simultaneous 0.5-10 keV X-ray and two-frequency radio observations at 2.25 and 8.3 GHz of the unusual binary system LSI+61 deg 303. This system was observed twice in a single binary orbit by the ASCA satellite, and monitored daily at two radio frequencies during the same orbital cycle with the Greenbank Interferometer. During the first ASCA observation the source was detected with a 1-10 keV luminosity 3.6 x 1033 (d/2.0 kpc )2 erg/s and during the second at a similar level with evidence for a decrease in average flux of 30%. During the first pointing the radio source was at a quiescent 8 GHz flux level of 30 mJy while during the second the radio flux was rising dramatically with an average value of 100 mJy. No variability is seen in the X-ray flux during the first pointing, but during the second the flux is variable by approx. 50% on timescales of approx. 30 minutes. No pulsations are seen in either X-ray observation with an upper limit on pulsed flux of 20% . The low X-ray luminosity and lack of observed pulsations indicate that accretion onto a neutron star surface is not the origin for the high-energy emission. Rather, the X-rays must result either from accreted matter which is stopped at the magnetosphere because the magnetospheric boundary is rotating at super-Keplerian rates or due to a shock formed in the interaction of the dense wind of the Be star companion and a moderately young pulsar.

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