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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.
Galaxies 2018, 6(1), 32;
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)
PDF [377 KB, uploaded 5 March 2018]


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

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