Hα EMISSION VARIABILITY IN THE γ-RAY BINARY LS I+61 303

被引：15

作者：

McSwain, M. Virginia ^{[1
]}

Grundstrom, Erika D. ^{[2
]}

Gies, Douglas R. ^{[3
]}

Ray, Paul S. ^{[4
]}

机构：

[1] Lehigh Univ, Dept Phys, Bethlehem, PA 18015 USA

[2] Vanderbilt Univ, Dept Phys & Astron, Stevens Ctr 6301, Nashville, TN 37235 USA

[3] Georgia State Univ, Dept Phys & Astron, Ctr High Angular Resolut Astron, Atlanta, GA 30303 USA

[4] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA

来源：

ASTROPHYSICAL JOURNAL | 2010年 / 724卷 / 01期

基金：

美国国家科学基金会;

关键词：

accretion; accretion disks; stars:; emission-line; Be; stars: individual (LS I+61 303); winds; outflows; X-RAY; RADIO OBSERVATIONS; LSI+61-DEGREES-303; STAR;

D O I：

10.1088/0004-637X/724/1/379

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

LS I +61 303 is an exceptionally rare example of a high-mass X-ray binary that also exhibits McV-TcV emission, making it one of only a handful of "gamma-ray binaries." Here we present H alpha spectra that show strong variability during the 26.5 day orbital period and over decadal timescales. We detect evidence of a spiral density wave in the Be circumstellar disk over part of the orbit. The H alpha line profile also exhibits a dramatic emission burst shortly before apastron, observed as a redshifted shoulder in the line profile, as the compact source moves almost directly away from the observer. We investigate several possible origins for this red shoulder, including an accretion disk, mass-transfer stream, and a compact pulsar wind nebula that forms via a shock between the Be star's wind and the relativistic pulsar wind.

引用

页码：379 / 385

页数：7

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