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Analysis of the X-ray emission of OB stars II: B stars. / Ryspaeva, Elizaveta ; Kholtygin, Alexander .

In: Research in Astronomy and Astrophysics, Vol. 19, No. 8, 120, 15.08.2019.

Research output: Contribution to journal › Article › peer-review

Harvard

Ryspaeva, E & Kholtygin, A 2019, 'Analysis of the X-ray emission of OB stars II: B stars', Research in Astronomy and Astrophysics, vol. 19, no. 8, 120. https://doi.org/10.1088/1674-4527/19/8/120

APA

Ryspaeva, E., & Kholtygin, A. (2019). Analysis of the X-ray emission of OB stars II: B stars. Research in Astronomy and Astrophysics, 19(8), [120]. https://doi.org/10.1088/1674-4527/19/8/120

Vancouver

Ryspaeva E, Kholtygin A. Analysis of the X-ray emission of OB stars II: B stars. Research in Astronomy and Astrophysics. 2019 Aug 15;19(8). 120. https://doi.org/10.1088/1674-4527/19/8/120

Author

Ryspaeva, Elizaveta ; Kholtygin, Alexander . / Analysis of the X-ray emission of OB stars II: B stars. In: Research in Astronomy and Astrophysics. 2019 ; Vol. 19, No. 8.

BibTeX

@article{e384d0dddaef41b181ebce819203c820,
title = "Analysis of the X-ray emission of OB stars II: B stars",
abstract = "This paper is the second part of an investigation into the mechanism for the origin of X-rays in early-type stars. Archival X-ray observations of 25 B stars, obtained by the XMM-Newton satellite, are analysed. We check two hypotheses on the origin of X-ray emission: the Magnetically Confined Wind Shock Model (MCWS) and Pollock's paradigm. For all studied stars, the mean ratio of the half widths at half maximum to the terminal velocities appears to be $R\approx 0.15-0.20$ in contradiction to Pollock's hypothesis that $R\approx 0.5$. We checked three possible consequences of the MCWS model: correlations between the hardness of the X-ray spectra for B stars and terminal wind velocities, mass loss rates and magnetic fields. It was shown that such correlations are marginal or even absent both for magnetic and non-magnetic B stars.",
keywords = "stars, early-type — stars, Spectra, X-Ray, stars: early-type, stars: spectra: X-ray, SHOCKS, PARADIGM",
author = "Elizaveta Ryspaeva and Alexander Kholtygin",
year = "2019",
month = aug,
day = "15",
doi = "10.1088/1674-4527/19/8/120",
language = "English",
volume = "19",
journal = "Research in Astronomy and Astrophysics",
issn = "1674-4527",
publisher = "IOP Publishing Ltd.",
number = "8",

}

RIS

TY - JOUR

T1 - Analysis of the X-ray emission of OB stars II: B stars

AU - Ryspaeva, Elizaveta

AU - Kholtygin, Alexander

PY - 2019/8/15

Y1 - 2019/8/15

N2 - This paper is the second part of an investigation into the mechanism for the origin of X-rays in early-type stars. Archival X-ray observations of 25 B stars, obtained by the XMM-Newton satellite, are analysed. We check two hypotheses on the origin of X-ray emission: the Magnetically Confined Wind Shock Model (MCWS) and Pollock's paradigm. For all studied stars, the mean ratio of the half widths at half maximum to the terminal velocities appears to be $R\approx 0.15-0.20$ in contradiction to Pollock's hypothesis that $R\approx 0.5$. We checked three possible consequences of the MCWS model: correlations between the hardness of the X-ray spectra for B stars and terminal wind velocities, mass loss rates and magnetic fields. It was shown that such correlations are marginal or even absent both for magnetic and non-magnetic B stars.

AB - This paper is the second part of an investigation into the mechanism for the origin of X-rays in early-type stars. Archival X-ray observations of 25 B stars, obtained by the XMM-Newton satellite, are analysed. We check two hypotheses on the origin of X-ray emission: the Magnetically Confined Wind Shock Model (MCWS) and Pollock's paradigm. For all studied stars, the mean ratio of the half widths at half maximum to the terminal velocities appears to be $R\approx 0.15-0.20$ in contradiction to Pollock's hypothesis that $R\approx 0.5$. We checked three possible consequences of the MCWS model: correlations between the hardness of the X-ray spectra for B stars and terminal wind velocities, mass loss rates and magnetic fields. It was shown that such correlations are marginal or even absent both for magnetic and non-magnetic B stars.

KW - stars

KW - early-type — stars

KW - Spectra

KW - X-Ray

KW - stars: early-type

KW - stars: spectra: X-ray

KW - SHOCKS

KW - PARADIGM

UR - http://www.raa-journal.org/docs/papers_accepted/2018-0366.pdf

UR - http://www.scopus.com/inward/record.url?scp=85072805365&partnerID=8YFLogxK

UR - http://www.mendeley.com/research/analysis-xray-emission-ob-stars-ii-b-stars

U2 - 10.1088/1674-4527/19/8/120

DO - 10.1088/1674-4527/19/8/120

M3 - Article

VL - 19

JO - Research in Astronomy and Astrophysics

JF - Research in Astronomy and Astrophysics

SN - 1674-4527

IS - 8

M1 - 120

ER -

ID: 48418137