The Pulsar Wind Nebula of the Geminga Pulsar

Details The Pulsar Wind Nebula of the Geminga Pulsar The Pulsar Wind Nebula of the Geminga Pulsar

Aug 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004head....8.1106s&link_type=abstract

American Astronomical Society, HEAD meeting #8, #11.06; Bulletin of the American Astronomical Society, Vol. 36, p.923

Astronomy and Astrophysics

Astronomy

1

Scientific paper

XMM-Newton observations of Geminga have shown two 2'-long, faint structures opposite to the direction of pulsar's proper motion. These structures have been interpreted as the tails of a bow-shock in the pulsar wind caused by the supersonic motion of the pulsar in the ambient ISM. This interpretation implies a stand-off distance for the bow-shock head of about 20''.
We have observed Geminga with the Chandra ACIS detector. Thanks to the superior spatial resolution of Chandra, we find a small ``wake'' right behind the pulsar, approximately 10''--15'' long. We also find enhanced emission ahead of the pulsar, about a factor of 30 brighter than the extended tails seen with XMM. If this is the head of the bow-shock, the implied stand-off distance is about 5''--7'', much smaller than implied by the XMM-Newton data.
We will present the spatial and spectral analysis of the X-ray nebula around the Gemimga pulsar and discuss the implications of the Chandra and XMM data.
This work was supported by SAO grant GO4-5083X and NASA grant NAG5-10865.

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