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Importance of electron-positron pairs on the maximum possible luminosity of the accretion columns in ULXs

Published online by Cambridge University Press:  27 February 2023

Valery F. Suleimanov Open the ORCID record for Valery F. Suleimanov [Opens in a new window] ,
Alexander Mushtukov ,
Igor Ognev ,
Victor A. Doroshenko  and
Klaus Werner
Valery F. Suleimanov
Affiliation:
Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, D-72076, Tübingen, Germany email: [email protected] Kazan Federal University, Kremlevskaya 18, 420008 Kazan, Russia Space Research Institute of the Russian Academy of Science, Profsoyuznaya 84/32, 117997 Moscow, Russia
Alexander Mushtukov
Affiliation:
Space Research Institute of the Russian Academy of Science, Profsoyuznaya 84/32, 117997 Moscow, Russia Leiden Observatory, Leiden University, NL-2300RA Leiden, the Netherlands
Igor Ognev
Affiliation:
P. G. Demidov Yaroslavl State University, Sovietskaya 14, 150003 Yaroslavl, Russia
Victor A. Doroshenko
Affiliation:
Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, D-72076, Tübingen, Germany email: [email protected] Space Research Institute of the Russian Academy of Science, Profsoyuznaya 84/32, 117997 Moscow, Russia
Klaus Werner
Affiliation:
Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, D-72076, Tübingen, Germany email: [email protected]
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Abstract

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One of the models explaining the high luminosity of pulsing ultra-luminous X-ray sources (pULXs) was suggested by Mushtukov et al. (2015). They showed that the accretion columns on the surfaces of highly magnetized neutron stars can be very luminous due to opacity reduction in the high magnetic field. However, a strong magnetic field leads also to amplification of the electron-positron pairs creation. Therefore, increasing of the electron and positron number densities compensates the cross-section reduction, and the electron scattering opacity does not decrease with the magnetic field magnification. As a result, the maximum possible luminosity of the accretion column does not increase with the magnetic field. It ranges between 1040 − 1041 erg s−1 depending only slightly on the magnetic field strength.

Keywords

accretionaccretion disksstars: neutronX-rays: binariesradiative transfer
Type
Poster Paper
Information
Proceedings of the International Astronomical Union , Volume 16 , Symposium S363: Neutron Star Astrophysics at the Crossroads: Magnetars and the Multimessenger Revolution , June 2020 , pp. 327 - 328
Creative Commons
Creative Common License - CCCreative Common License - BY
This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution, and reproduction in any medium, provided the original work is properly cited.
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

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