The clumpy absorber in the high-mass X-ray binary Vela X-1

被引：37

作者：

Grinberg, V. ^{[1
]}

Hell, N. ^{[2
]}

El Mellah, I. ^{[3
]}

Neilsen, J. ^{[4
]}

Sander, A. A. C. ^{[5
]}

Leutenegger, M. ^{[6
,7
,8
]}

Furst, F. ^{[9
]}

Huenemoerder, D. P. ^{[10
]}

Kretschmar, P. ^{[9
]}

Kuehnel, M. ^{[11
,12
]}

Martinez-Nunez, S. ^{[13
]}

Niu, S. ^{[11
,12
,14
]}

Pottschmidt, K. ^{[6
,7
,8
]}

Schulz, N. S. ^{[10
]}

Wilms, J. ^{[11
,12
]}

Nowak, M. A. ^{[10
]}

机构：

[1] ESA, European Space Res & Technol Ctr ESTEC, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands

[2] Lawrence Livermore Natl Lab, 7000 East Ave, Livermore, CA 94550 USA

[3] Katholieke Univ Leuven, Dept Math, Ctr Math Plasma Astrophys, Celestijnenlaan 200B, B-3001 Leuven, Belgium

[4] Villanova Univ, Dept Phys, Villanova, PA 19085 USA

[5] Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany

[6] UMBC, Dept Phys, CRESST, Baltimore, MD 21250 USA

[7] UMBC, Ctr Space Sci & Technol, Baltimore, MD 21250 USA

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

[9] ESA, European Space Astron Ctr ESAC, Sci Operat Dept, Madrid 28692, Spain

[10] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA

[11] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte, D-96049 Bamberg, Germany

[12] Univ Erlangen Nurnberg, ECAP, D-96049 Bamberg, Germany

[13] Univ Cantabria, CSIC, Inst Fis Cantabria, E-39005 Santander, Spain

[14] Chinese Acad Sci, Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China

来源：

ASTRONOMY & ASTROPHYSICS | 2017年 / 608卷

关键词：

X-rays: individuals: Vela X-1; X-rays: binaries; stars:; winds; outflows; stars: massive; HELIUM-LIKE IONS; STELLAR WIND; LABORATORY MEASUREMENTS; CIRCUMSTELLAR MATTER; LINE-INTENSITIES; K-LINES; SPECTROSCOPY; ABSORPTION; SUPERGIANT; EMISSION;

D O I：

10.1051/0004-6361/201731843

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Bright and eclipsing, the high-mass X-ray binary Vela X-1 offers a unique opportunity to study accretion onto a neutron star from clumpy winds of O/B stars and to disentangle the complex accretion geometry of these systems. In Chandra-HETGS spectroscopy at orbital phase similar to 0.25, when our line of sight towards the source does not pass through the large-scale accretion structure such as the accretion wake, we observe changes in overall spectral shape on timescales of a few kiloseconds. This spectral variability is, at least in part, caused by changes in overall absorption and we show that such strongly variable absorption cannot be caused by unperturbed clumpy winds of O/B stars. We detect line features from high and low ionization species of silicon, magnesium, and neon whose strengths and presence depend on the overall level of absorption. These features imply a co-existence of cool and hot gas phases in the system, which we interpret as a highly variable, structured accretion flow close to the compact object such as has been recently seen in simulations of wind accretion in high-mass X-ray binaries.

引用

页数：18

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