C.D.S. - SIMBAD4 rel 1.7 - 2019.07.16CEST19:21:32

2016A&A...587A..63V - Astronomy and Astrophysics, volume 587A, 63-63 (2016/3-1)

Modeling the polarization of high-energy radiation from accreting black holes. A case study of XTE J1118+480.


Abstract (from CDS):

The high-energy emission (400keV-2MeV) of Cygnus X-1, which is the best-studied Galactic black hole, was recently found to be strongly polarized. The origin of this radiation is still unknown. We suggest that the emission is the result of non-thermal processes in the hot corona around the accreting compact object and study the polarization of high-energy radiation that is expected for black hole binaries. Two contributions to the total magnetic field were taken into account in our study: a small-scale random component related to the corona, and an ordered magnetic field associated with the accretion disk. The degree of polarization of gamma-ray emission for this particular geometry was estimated together with the angle of the polarization vector. We obtain that the configuration of corona plus disk can account for the high degree of polarization of gamma-rays that are detected in galactic black holes and does not need to invoke a relativistic jet. We make specific predictions for sources in a low-hard state. In particular, the model is applied to the transient source XTEJ1118+480. We show that if a new outburst of XTEJ1118+480 is observed, then its gamma-ray polarization should be measurable by future instruments, such as ASTRO-H or the proposed ASTROGAM.

Abstract Copyright:

Journal keyword(s): X-rays: binaries - gamma rays: general - polarization - stars: individual: XTE J1118+480

Simbad objects: 3

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Number of rows : 3

N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
1 NAME Lockman Hole reg 10 45 00.0 +58 00 00           ~ 730 0
2 V* KV UMa HXB 11 18 10.7922353051 +48 02 12.319175505     12.25     K5V-M1V 701 0
3 HD 226868 HXB 19 58 21.6758193269 +35 12 05.782512305 9.38 9.72 8.91 8.42   O9.7Iabpvar 3829 0

    Equat.    Gal    SGal    Ecl

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