The X-ray structure and spectrum of the pulsar wind nebula surrounding PSR B1853+01 in W44

被引：55

作者：

Petre, R ^{[1
]}

Kuntz, KD

Shelton, RL

机构：

[1] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[2] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA

来源：

ASTROPHYSICAL JOURNAL | 2002年 / 579卷 / 01期

关键词：

ISM : individual (W44); pulsars : individual (PSR B1853+01); supernova remnants; X-rays : general;

D O I：

10.1086/342672

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the result of a Chandra ACIS observation of the pulsar PSR B1853+01 and its associated pulsar wind nebula (PWN), embedded in the supernova remnant W44. A hard-band ACIS map cleanly distinguishes the PWN from the thermal emission of W44. The nebula is extended in the north-south direction, with an extent about half that of the radio emission. Morphological differences between the X-ray and radio images are apparent. Spectral fitting reveals a clear difference in spectral index between the hard emission from PSR B1853+01 (Gamma similar to 1.4) and the extended nebula (Gamma similar to 2.2). The more accurate values for the X-ray flux and spectral index are used to refine estimates for PWN parameters, including magnetic field strength, the average Lorentz factor gamma of the particles in the wind, the magnetization parameter sigma, and the ratio k of electrons to other particles.

引用

页码：404 / 410

页数：7

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