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Galaxies 2018, 6(1), 32; doi:10.3390/galaxies6010032

Studying Microquasars with X-Ray Polarimetry

Dipartimento di Matematica e Fisica, Università degli Studi Roma Tre, via della Vasca Navale 84, 00146 Roma, Italy
Astronomical Institute of the Czech Academy of Sciences, CZ-141 31 Prague Czech Republic
Author to whom correspondence should be addressed.
Received: 29 January 2018 / Revised: 26 February 2018 / Accepted: 27 February 2018 / Published: 5 March 2018
(This article belongs to the Special Issue The Bright Future of Astronomical X-ray Polarimetry)
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Microquasars are Galactic black hole systems in which matter is transferred from a donor star and accretes onto a black hole of, typically, 10–20 solar masses. The presence of an accretion disk and a relativistic jet made them a scaled down analogue of quasars—thence their name. Microquasars feature prominently in the scientific goals of X-ray polarimeters, because a number of open questions, which are discussed in this paper, can potentially be answered: the geometry of the hot corona believed to be responsible for the hard X-ray emission; the role of the jet; the spin of the black hole. View Full-Text
Keywords: X-ray polarimetry; microquasars; Comptonization X-ray polarimetry; microquasars; Comptonization

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This is an open access article distributed under the Creative Commons Attribution License which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. (CC BY 4.0).

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Matt, G.; Tamborra, F. Studying Microquasars with X-Ray Polarimetry. Galaxies 2018, 6, 32.

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