Imaging the binary plerion

Details Imaging the binary plerion Imaging the binary plerion

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008cxo..prop.2587p&link_type=abstract

Chandra proposal ID #10500440

Computer Science

Scientific paper

The radio pulsar B1259-63 is in an eccentric binary (e=0.87, P=3.4 yr) with a high-mass Be companion. Being dependent on binary orbital phase, the X-ray emission of this system is believed to be generated in a bow-shock pulsar wind nebula (PWN) formed by colliding winds from the pulsar and the companion. However, this very compact PWN has never been resolved in previous low-resolution observations. Imaging the B1259-63 PWN with the ACIS detector, we expect to detect a PWN tail, similar to those commonly observed behind solitary pulsars moving in the ISM with supersonic speeds, and a pulsar jet. Studying the properties of this unusual PWN will help to understand the nature of stellar and pulsar winds and their interaction.

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