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On the origin of Supergiant Fast X-ray Transients

Published online by Cambridge University Press:  30 December 2019

Swetlana Hubrig ,
Lara Sidoli ,
Konstantin A. Postnov ,
Markus Schöller ,
Alexander F. Kholtygin  and
Silva P. Järvinen
Swetlana Hubrig
Affiliation:
Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany email: [email protected]
Lara Sidoli
Affiliation:
INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica, Via E. Bassini 15, 20133 Milano, Italy
Konstantin A. Postnov
Affiliation:
Sternberg Astronomical Institute, Moscow M.V. Lomonosov State University, 119234 Moscow, Russia
Markus Schöller
Affiliation:
European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany
Alexander F. Kholtygin
Affiliation:
Saint-Petersburg State University, Universitetskij pr. 28, 198504 Saint-Petersburg, Russia
Silva P. Järvinen
Affiliation:
Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany email: [email protected]
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Abstract

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. 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: magnetic fieldsstars: individual (IGR J08408–4503IGR J11215-5952)(stars:) supergiants(stars:) binaries: generalX-rays: stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S346: High-mass X-ray Binaries: Illuminating the Passage from Massive Binaries to Merging Compact Objects , August 2018 , pp. 193 - 196
Copyright
© International Astronomical Union 2019 

References

Appenzeller, I., Fricke, K., Fürtig, W., Gässler, W., Häfner, R., Harke, R., Hess, H.-J., Hummel, W., Jürgens, P., Kudritzki, R.-P., Mantel, K.-H., Meisl, W., Muschielok, B., Nicklas, H., Rupprecht, G., Seifert, W., Stahl, O., Szeifert, T., & Tarantik, K. 1998, The ESO Messenger, 94, 1 Google Scholar
Hubrig, S., Schöller, M., Schnerr, R.S., González, J. F., Ignace, R., & Henrichs, H. 2008, A&A, 490, 793 Google Scholar
Hubrig, S., Schöller, M., Kharchenko, N. V., Langer, N., de Wit, W. J., Ilyin, I., Kholtygin, A. F., Piskunov, A. E., Przybilla, N., & Collaboration, Magori 2011, A&A, 528, A151 Google Scholar
Hubrig, S., Sidoli, L., Postnov, K., Schöller, M., Kholtygin, A. F., Järvinen, S. P., & Steinbrunner, P. 2018, MNRAS, 474, L27 CrossRefGoogle Scholar
Lorenzo, J., Negueruela, I., Castro, N., Norton, A. J., Vilardell, F., & Herrero, A. 2014, A&A, 562, A18 Google Scholar
Martinez-Nunez, S., Kretschmar, P., Bozzo, E., Oskinova, L. M., Puls, J., Sidoli, L., Sundqvist, J. O., Blay, P., Falanga, M., Fürst, F., Gímenez-García, A., Kreykenbohm, I., Kühnel, M., Sander, A., Torrejón, J. M., & Wilms, J. 2017, SSRv, 212, 59 Google Scholar
Persi, P., Fiocchi, M., Tapia, M., Roth, M., Bazzano, A., Ubertini, P., & Parisi, P. 2015, AJ, 150, 21 CrossRefGoogle Scholar
Postnov, K. A., Gornostaev, M. I., Klochkov, D., Laplace, E., Lukin, V. V., & Shakura, N. I. 2015, MNRAS, 452, 1601 CrossRefGoogle Scholar
Romano, P., Sidoli, L., Cusumano, G., Vercellone, S., Mangano, V., & Krimm, H. A. 2009, ApJ, 696, 2068 CrossRefGoogle Scholar
Shakura, N., Postnov, K., Sidoli, L., & Paizis, A. 2014, MNRAS, 420, 216 CrossRefGoogle Scholar
Shakura, N. I., Postnov, K. A., Kochetkova, A. Yu., Hjalmarsdotter, L., Sidoli, L., & Paizis, A. 2015. ARep, 59, 645 Google Scholar
Shakura, N., & Postnov, K. 2017, Accretion Processes in Cosmic Sources, September 5-10, 2016, St-Petersburg, also: arXiv:1702.03393Google Scholar
Sidoli, L., Paizis, A., & Mereghetti, S. 2006, A&A, 450, L9 Google Scholar
Sidoli, L., Romano, P., Mereghetti, S., Paizis, A, Vercellone, S., Mangano, V., & Götz, D. 2007, A&A, 476, 1307 Google Scholar
Sidoli, L. 2017, Proc. of the “XII Multifrequency Behaviour of High Energy Cosmic Sources Workshop”, 12-17 June, 2017 Palermo, Italy, 52Google Scholar
van den Heuvel, E. P. J., & Heise, J. 1972, Nature Physical Science, 239, 67 CrossRefGoogle Scholar
ud-Doula, A. , & Owocki, S. P. 2002, ApJ, 576, 413 CrossRefGoogle Scholar