2009A&A...497..325B


C.D.S. - SIMBAD4 rel 1.7 - 2020.08.14CEST02:07:49

2009A&A...497..325B - Astronomy and Astrophysics, volume 497, 325-334 (2009/4-2)

Non-thermal emission from microquasar/ISM interaction.

BORDAS P., BOSCH-RAMON V., PAREDES J.M. and PERUCHO M.

Abstract (from CDS):

The interaction of microquasar jets with their environment can produce non-thermal radiation as in the case of extragalactic outflows impacting on their surroundings. Significant observational evidence of jet/medium interaction in galactic microquasars has been collected in the past few years, although little theoretical work has been done regarding the resulting non-thermal emission. In this work, we investigate the non-thermal emission produced in the interaction between microquasar jets and their environment, and the physical conditions for its production. We developed an analytical model based on those successfully applied to extragalactic sources. The jet is taken to be a supersonic and mildly relativistic hydrodynamical outflow. We focus on the jet/shocked medium structure in its adiabatic phase, and assume that it grows in a self-similar way. We calculate the fluxes and spectra of the radiation produced via synchrotron, inverse Compton, and relativistic bremsstrahlung processes by electrons accelerated in strong shocks. A hydrodynamical simulation is also performed to investigate further the jet interaction with the environment and check the physical parameters used in the analytical model. For reasonable values of the magnetic field, and using typical values of the external matter density, the non-thermal particles could produce significant amounts of radiation at different wavelengths, although they do not cool primarily radiatively, but by adiabatic losses. The physical conditions of the analytical jet/medium interaction model are consistent with those found in the hydrodynamical simulation. Microquasar jet termination regions could be detectable at radio wavelengths for current instruments sensitive to ∼arcminute scales. At X-ray energies, the expected luminosities are moderate, although the emitter is more compact than the radio one. The source may be detectable by XMM-Newton or Chandra, with 1-10arcsec of angular resolution. The radiation at gamma-ray energies may be within the detection limits of the next generation of satellite and ground-based instruments.

Abstract Copyright:

Journal keyword(s): ISM: jets and outflows - X-rays: binaries - radiation mechanisms: non-thermal

Simbad objects: 9

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Number of rows : 9

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 LS I +61 303 HXB 02 40 31.6641883136 +61 13 45.591138110 11.27 11.61 10.75 10.19 9.55 B0Ve 762 2
2 V* BR Cir HXB 15 20 40.85 -57 10 00.1   21.4 21.4     ~ 723 1
3 V* V381 Nor HXB 15 50 58.6520652623 -56 28 35.309070422   17.95 16.6     K3III 1028 0
4 NAME Great Annihilator LXB 17 43 54.83 -29 44 42.6           ~ 639 1
5 NAME XTE J17464-3213 LXB 17 46 15.59637 -32 14 00.8600           ~ 602 0
6 SS 433 HXB 19 11 49.5645897701 +04 58 57.824087535   16.3 13.0     A7Ib: 1937 3
7 Granat 1915+105 LXB 19 15 11.54938 +10 56 44.7585           ~ 2293 0
8 HD 226868 HXB 19 58 21.6758193269 +35 12 05.782512305 9.38 9.72 8.91 8.42   O9.7Iabpvar 3935 0
9 V* V1521 Cyg HXB 20 32 25.78 +40 57 27.9           WN4/5-6/7 1768 2

    Equat.    Gal    SGal    Ecl

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2020.08.14-02:07:49

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