Chandra observations of the pulsar wind nebula in supernova remnant G0.9+0.1

被引：45
作者：
Gaensler, BM
Pivovaroff, MJ
Garmire, GP
机构：
[1] MIT, Ctr Space Res, Cambridge, MA 02139 USA
[2] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA
来源：
ASTROPHYSICAL JOURNAL | 2001年 / 556卷 / 02期
基金：
美国国家航空航天局;
关键词：
ISM : individual (G0.9+0.1); pulsars : general; stars; winds; outflows; supernova remnants;
D O I：
10.1086/322982
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We present observations with the Chandra X-Ray Observatory of the pulsar wind nebula (PWN) within the supernova remnant G0.9+0.1. At Chandra's high resolution, the PWN has a clear axial symmetry; a faint X-ray point source lying along the symmetry axis possibly corresponds to the pulsar itself. We argue that the nebular morphology can be explained in terms of a torus of emission in the pulsar's equatorial plane and a jet directed along the pulsar spin axis, as is seen in the X-ray nebulae powered by other young pulsars. A bright clump of emission within the PWN breaks the axisymmetry and may correspond to an intermediate-latitude feature in the pulsar wind.
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收藏
页码：L107 / L111
页数：5
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