2003A&A...399.1121B


C.D.S. - SIMBAD4 rel 1.7 - 2020.04.05CEST21:57:00

2003A&A...399.1121B - Astronomy and Astrophysics, volume 399, 1121-1134 (2003/3-1)

Gamma-ray emission from Wolf-Rayet binaries.

BENAGLIA P. and ROMERO G.E.

Abstract (from CDS):

In the colliding wind region of early-type binaries, electrons can be accelerated up to relativistic energies displaying power-law spectra, as demonstrated by the detection of non-thermal radio emission from several WR+OB systems. The particle acceleration region, located between the stars, is exposed to strong photon fields in such a way that inverse Compton cooling of the electrons could result in a substantial high-energy non-thermal flux. In particular cases, the ratio of the energy densities of magnetic to photon fields in the colliding wind region will determine whether a given source can produce or not significant gamma-ray emission. We present here a study of the binaries WR 140, WR 146, and WR 147 in the light of recent radio and gamma-ray observations. We show that with reasonable assumptions for the magnetic field strength WR 140 can produce the gamma-ray flux from the EGRET source 3EG J2022+4317. WR 146 and WR 147 are below the detection threshold, but new and forthcoming instruments like INTEGRAL and GLAST might detect non-thermal emission from them.

Abstract Copyright:

Journal keyword(s): stars: early-type - stars: binaries: general - stars: winds, outflows - radio continuum: stars - gamma-rays: observations - gamma-rays: theory

Status at CDS:  

Simbad objects: 17

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Number of rows : 17

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 * gam02 Vel WR* 08 09 31.95013 -47 20 11.7108 0.64 1.58 1.83 1.85 2.00 WC8+O7.5III-V 834 0
2 HD 76536 WR* 08 54 59.1670924993 -47 35 32.662255423 9.04 9.13 8.80 9.52   WC 111 0
3 WR 39 WR* 11 06 18.7256631005 -61 14 18.428457304   14.33 13.05 13.15   WC7 40 0
4 * tet Mus WR* 13 08 07.1527888825 -65 18 21.679641155 4.71 5.50 5.53 5.44 5.40 WC5+B0III 294 0
5 HD 156385 WR* 17 19 29.9012727857 -45 38 23.874796927 6.55 6.97 6.92 8.11   WC7 151 0
6 EM* AS 268 WR* 18 02 23.4579211710 -23 34 37.481060535   14.38 12.31 11.43   WN9h 95 0
7 WR 112 WR* 18 16 33.49 -18 58 42.3   20.7 17.7     WC8+O6/7III/V 116 0
8 MR 93 WR* 19 28 15.6144084163 +19 33 21.527872339   14.83       WC7+O9(III) 100 0
9 HD 192641 WR* 20 14 31.7667382048 +36 39 39.597237795 7.80 8.20 7.91     WC7+O9 302 0
10 HD 193793 WR* 20 20 27.9763345925 +43 51 16.289775091 6.90 7.25 6.85 4.58   WC7p+O5 645 1
11 3EG J2022+4317 gam 20 22 +43.3           ~ 20 0
12 BD+40 4220 EB* 20 32 22.4241357648 +41 18 18.942382590 11.32 10.79 9.185     O6.5-7f+O5.5-6f 366 0
13 Ass Cyg OB 2 As* 20 33.2 +41 19           ~ 776 0
14 MR 112 WR* 20 35 47.0859278605 +41 22 44.703520146     12.64 12.16   WC5-6e+O8 138 1
15 [MDB89] AS 431 S * 20 36 30.0530051342 +40 21 23.024435829           WN8 8 0
16 EM* AS 431 WR* 20 36 43.6 +40 21 08   17.04 14.89     WN8(h)+B0.5V 204 2
17 NAME WR 147 NIR * 20 36 43.6 +40 21 14   20.11 16.02     B0.5V 7 0

    Equat.    Gal    SGal    Ecl

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2020.04.05-21:57:00

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