Periastron Observations of a Massive Eclipsing Pulsar Binary System

Details Periastron Observations of a Massive Eclipsing Pulsar Binary System Periastron Observations of a Massive Eclipsing Pulsar Binary System

Sep 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004cxo..prop.1862m&link_type=abstract

Chandra Proposal ID #06408206

Astronomy and Astrophysics

Astronomy

1

Chandra Proposal Id #06408206

Scientific paper

The 764-ms pulsar J1638-4725 is in an eccentric (e ~ 0.94) orbit with a 5.3-yr period about a ~ 20 solar mass optically-identified companion. The pulsar is undetectable in the radio for ~ 1 yr around periastron, most likely due to absorption and scattering by the dense stellar environment. During this radio-quiet phase, X-rays from the "propeller regime" accretion of matter onto the NS magnetosphere are likely to be detectable. If such emission is detected near periastron (April 30 2005), this binary will be the first system in which an accretion phase alternates with a radio pulsar phase, providing a link between the populations of X-ray transients and radio pulsars and an important diagnostic of the companion star mass loss rate and its terminal velocity (and hence mass and radius). X-rays may also be detected from the pulsar, the companion star, and pulsar wind/disk shock but are expected to be an order of magnitude less than that expected from propeller accretion.

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