Sokal 2010 Chandra对WR星WR 142和OB星的观测

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WR极有可能是伽马暴的前身星。

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Title:		Chandra Detects the Rare Oxygen-type Wolf-Rayet Star WR 142 and OB Stars in Berkeley 87
Authors:		Sokal, Kimberly R.; Skinner, Stephen L.; Zhekov, Svetozar A.; Güdel, Manuel; Schmutz, Werner
Affiliation:		AA(CASA, University of Colorado, Boulder, CO 80309-0389, USA kimberly.sokal@colorado.edu), AB(CASA, University of Colorado, Boulder, CO 80309-0389, USA stephen.skinner@colorado.edu), AC(JILA, University of Colorado, Boulder, CO 80309-0440, USA ; On leave from Space Research Institute, Sofia, Bulgaria.), AD(Department of Astronomy, University of Vienna, Türkenschanzstr. 17, A-1180 Vienna, Austria ), AE(Physikalisch-Meteorologisches Observatorium Davos and World Radiation Center (PMOD/WRC), Dorfstrasse 33, CH-7260 Davos Dorf, Switzerland )
Publication:		The Astrophysical Journal, Volume 715, Issue 2, pp. 1327-1337 (2010). (ApJ Homepage)
Publication Date:		06/2010
Origin:		IOP
ApJ Keywords:		open clusters and associations: individual: Berkeley 87, stars: individual: WR 16 WR 142 &equals Sand 5 &equals St 3 BD+36 4032 HD 229059 V439 Cyg, stars: Wolf-Rayet, X-rays: stars
DOI:		10.1088/0004-637X/715/2/1327
Bibliographic Code:		2010ApJ...715.1327S

Abstract

We present first results of a Chandra X-ray observation of the rare oxygen-type Wolf-Rayet (WR) star WR 142 (= Sand 5 = St 3) harbored in the young, heavily obscured cluster Berkeley 87. Oxygen-type WO stars are thought to be the most evolved of the WRs and progenitors of supernovae or gamma-ray bursts. As part of an X-ray survey of supposedly single WR stars, we observed WR 142 and the surrounding Berkeley 87 region with Chandra ACIS-I. We detect WR 142 as a faint yet extremely hard X-ray source. Due to weak emission, its nature as a thermal or non-thermal emitter is unclear and thus we discuss several emission mechanisms. Additionally, we report seven detections and eight non-detections by Chandra of massive OB stars in Berkeley 87, two of which are bright yet soft X-ray sources whose spectra provide a dramatic contrast to the hard emission from WR 142.

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