Chandra Observations Of The Pulsar Psr B1929+10 And Its Environment

Details Chandra Observations Of The Pulsar Psr B1929+10 And Its Environment Chandra Observations Of The Pulsar Psr B1929+10 And Its Environment

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006head....9.0758m&link_type=abstract

American Astronomical Society, HEAD meeting #9, #7.58; Bulletin of the American Astronomical Society, Vol. 38, p.359

Astronomy and Astrophysics

Astronomy

1

Scientific paper

Pulsar wind nebulae (PWNe) are generated by
pulsar winds interacting with the ambient medium.
Most of the detected PWNe are produced by young, energetic pulsars,
often showing jets and torus-like structures or bow-shock structures caused
by the pulsar's motion. Only a few PWNe have been
detected around
middle-aged and
old pulsars.
the most intriguing
being a long ( 1.6 pc), trail-like extended structure
behind the 3-million-year old pulsar PSR B1929+10. ROSAT and XMM-Newton
observations have suggested
that this extended emission is most probably
synchrotron radiation from the pulsar wind
confined by the high ram pressure of the oncoming ISM,
but its association with the pulsar have not been firmly established yet.
We present two high-resolution Chandra ACIS-S
observations of PSR B1929+10, which reveal faint bow-shock-shaped extended
emission in the immediate vicinity of
PSR B1929+10
and a hint of a trail behind the pulsar.
The shape of the observed PWN suggests
that the pulsar wind is intrinsically anisotropic,
similar to the recently discovered PWN of the Geminga pulsar.
Furthermore, our data
indicate that the detected PWN emission is variable.
Although detected only in a small number of pulsars so far, the
bow-shock PWNe surrounding old pulsars provide an excellent opportunity to
probe pulsar winds and their interaction with the surrounding medium
at late stages of pulsar evolution.
This work was supported by NASA grants NAG5-10865 and NAS8-01128
and Chandra award SV4-74018.

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