8th HEAD Meeting, 8-11 September, 2004
Session 11 Pulsars and Magnetars
Oral, Wednesday, September 8, 2004, 4:00-5:30pm

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[11.06] The Pulsar Wind Nebula of the Geminga Pulsar

D. Sanwal, G. G. Pavlov (Pennsylvania State University), V. E. Zavlin (Strasbourg Astronomical Observatory)

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.

The author(s) of this abstract have provided an email address for comments about the abstract: divas@astro.psu.edu

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© 2004. The American Astronomical Soceity.