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On the origin of Supergiant Fast X-ray Transients. / Hubrig, Swetlana; Sidoli, Lara; Postnov, Konstantin A.; Schöller, Markus; Kholtygin, Alexander F.; Järvinen, Silva P.

в: Proceedings of the International Astronomical Union, 01.01.2019, стр. 193-196.

Результаты исследований: Научные публикации в периодических изданиях › статья › Рецензирование

Harvard

Hubrig, S, Sidoli, L, Postnov, KA, Schöller, M, Kholtygin, AF & Järvinen, SP 2019, 'On the origin of Supergiant Fast X-ray Transients', Proceedings of the International Astronomical Union, стр. 193-196. https://doi.org/10.1017/S1743921318008426

APA

Hubrig, S., Sidoli, L., Postnov, K. A., Schöller, M., Kholtygin, A. F., & Järvinen, S. P. (Принято в печать). On the origin of Supergiant Fast X-ray Transients. Proceedings of the International Astronomical Union, 193-196. https://doi.org/10.1017/S1743921318008426

Vancouver

Hubrig S, Sidoli L, Postnov KA, Schöller M, Kholtygin AF, Järvinen SP. On the origin of Supergiant Fast X-ray Transients. Proceedings of the International Astronomical Union. 2019 Янв. 1;193-196. https://doi.org/10.1017/S1743921318008426

Author

Hubrig, Swetlana ; Sidoli, Lara ; Postnov, Konstantin A. ; Schöller, Markus ; Kholtygin, Alexander F. ; Järvinen, Silva P. / On the origin of Supergiant Fast X-ray Transients. в: Proceedings of the International Astronomical Union. 2019 ; стр. 193-196.

BibTeX

@article{90e434d64d25465c9e69f8f2cc82fed1,
title = "On the origin of Supergiant Fast X-ray Transients",
abstract = "A fraction of high-mass X-ray binaries are supergiant fast X-ray transients. These systems have on average low X-ray luminosities, but display short flares during which their X-ray luminosity rises by a few orders of magnitude. The leading model for the physics governing this X-ray behaviour suggests that the winds of the donor OB supergiants are magnetized. In agreement with this model, the first spectropolarimetric observations of the SFXT IGR J11215-5952 using the FORS 2 instrument at the Very Large Telescope indicate the presence of a kG longitudinal magnetic field. Based on these results, it seems possible that the key difference between supergiant fast X-ray transients and other high-mass X-ray binaries are the properties of the supergiant's stellar wind and the physics of the wind's interaction with the neutron star magnetosphere.",
keywords = "(stars:) binaries: general, (stars:) supergiants, IGR J11215-5952), stars: individual (IGR J08408-4503, stars: magnetic fields, X-rays: stars",
author = "Swetlana Hubrig and Lara Sidoli and Postnov, {Konstantin A.} and Markus Sch{\"o}ller and Kholtygin, {Alexander F.} and J{\"a}rvinen, {Silva P.}",
year = "2019",
month = jan,
day = "1",
doi = "10.1017/S1743921318008426",
language = "English",
pages = "193--196",
journal = "Proceedings of the International Astronomical Union",
issn = "1743-9213",
publisher = "Cambridge University Press",

}

RIS

TY - JOUR

T1 - On the origin of Supergiant Fast X-ray Transients

AU - Hubrig, Swetlana

AU - Sidoli, Lara

AU - Postnov, Konstantin A.

AU - Schöller, Markus

AU - Kholtygin, Alexander F.

AU - Järvinen, Silva P.

PY - 2019/1/1

Y1 - 2019/1/1

N2 - A fraction of high-mass X-ray binaries are supergiant fast X-ray transients. These systems have on average low X-ray luminosities, but display short flares during which their X-ray luminosity rises by a few orders of magnitude. The leading model for the physics governing this X-ray behaviour suggests that the winds of the donor OB supergiants are magnetized. In agreement with this model, the first spectropolarimetric observations of the SFXT IGR J11215-5952 using the FORS 2 instrument at the Very Large Telescope indicate the presence of a kG longitudinal magnetic field. Based on these results, it seems possible that the key difference between supergiant fast X-ray transients and other high-mass X-ray binaries are the properties of the supergiant's stellar wind and the physics of the wind's interaction with the neutron star magnetosphere.

AB - A fraction of high-mass X-ray binaries are supergiant fast X-ray transients. These systems have on average low X-ray luminosities, but display short flares during which their X-ray luminosity rises by a few orders of magnitude. The leading model for the physics governing this X-ray behaviour suggests that the winds of the donor OB supergiants are magnetized. In agreement with this model, the first spectropolarimetric observations of the SFXT IGR J11215-5952 using the FORS 2 instrument at the Very Large Telescope indicate the presence of a kG longitudinal magnetic field. Based on these results, it seems possible that the key difference between supergiant fast X-ray transients and other high-mass X-ray binaries are the properties of the supergiant's stellar wind and the physics of the wind's interaction with the neutron star magnetosphere.

KW - (stars:) binaries: general

KW - (stars:) supergiants

KW - IGR J11215-5952)

KW - stars: individual (IGR J08408-4503

KW - stars: magnetic fields

KW - X-rays: stars

UR - http://www.scopus.com/inward/record.url?scp=85077459374&partnerID=8YFLogxK

U2 - 10.1017/S1743921318008426

DO - 10.1017/S1743921318008426

M3 - Article

AN - SCOPUS:85077459374

SP - 193

EP - 196

JO - Proceedings of the International Astronomical Union

JF - Proceedings of the International Astronomical Union

SN - 1743-9213

ER -

ID: 52919591