2020A&A...641A..84M


C.D.S. - SIMBAD4 rel 1.7 - 2020.12.05CET01:17:23

2020A&A...641A..84M - Astronomy and Astrophysics, volume 641A, 84-84 (2020/9-1)

A dynamical and radiation semi-analytical model of pulsar-star colliding winds along the orbit: Application to LS 5039.

MOLINA E. and BOSCH-RAMON V.

Abstract (from CDS):


Context. Gamma-ray binaries are systems that emit nonthermal radiation peaking at energies above 1 MeV. One proposed scenario to explain their emission consists of a pulsar orbiting a massive star, with particle acceleration taking place in shocks produced by the interaction of the stellar and pulsar winds.
Aims. We develop a semi-analytical model of the nonthermal emission of the colliding-wind structure, which includes the dynamical effects of orbital motion. We apply the model to a general case and to LS 5039.
Methods. The model consists of a one-dimensional emitter, the geometry of which is affected by Coriolis forces owing to orbital motion. Two particle accelerators are considered: one at the two-wind standoff location and the other one at the turnover produced by the Coriolis force. Synchrotron and inverse Compton emission is studied taking into account Doppler boosting and absorption processes associated to the massive star.
Results. If both accelerators are provided with the same energy budget, most of the radiation comes from the region of the Coriolis turnover and beyond, up to a few orbital separations from the binary system. Significant orbital changes of the nonthermal emission are predicted in all energy bands. The model allows us to reproduce some of the LS 5039 emission features, but not all of them. In particular, the MeV radiation is probably too high to be explained by our model alone, the GeV flux is recovered but not its modulation, and the radio emission beyond the Coriolis turnover is too low. The predicted system inclination is consistent with the presence of a pulsar in the binary.
Conclusions. The model is quite successful in reproducing the overall nonthermal behavior of LS 5039. Some improvements are suggested to better explain the phenomenology observed in this source, such as accounting for particle reacceleration beyond the Coriolis turnover, unshocked pulsar wind emission, and the three-dimensional extension of the emitter.

Abstract Copyright: © ESO 2020

Journal keyword(s): gamma rays: stars - radiation mechanisms: non-thermal - stars: winds, outflows - stars: individual: LS 5039

Simbad objects: 11

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Number of rows : 11

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#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 768 2
2 CXOU J053600.0-673507 X 05 36 00.01 -67 35 07.5           ~ 21 0
3 HD 259440 HXB 06 32 59.2566624297 +05 48 01.162565528 9.17 9.58 9.12     B0pe 190 0
4 3FHL J1018.8-5857 HXB 10 19 02.270 -58 56 29.87           ~ 94 0
5 CPD-63 2495 HXB 13 02 47.6541729594 -63 50 08.625922862 10.34 10.72 9.98 10.03   O9.5Ve 684 1
6 1FGL J1405.1-6123c gam 14 05 12 -61 23.7           ~ 24 0
7 V* V479 Sct HXB 18 26 15.0561532140 -14 50 54.249464136 12.02 12.23 11.27 11.04   ON6V((f))z 497 2
8 NAME XMMU J183245-0921539 XB* 18 32 45.162 -09 21 54.55           ~ 15 0
9 HD 226868 HXB 19 58 21.6758193269 +35 12 05.782512305 9.38 9.72 8.91 8.42   O9.7Iabpvar 3960 0
10 [MT91] 213 Be* 20 32 13.1248987067 +41 27 24.343749507 13.12 13.08 11.266     B0Vp 221 0
11 V* V1521 Cyg HXB 20 32 25.78 +40 57 27.9           WN4/5-6/7 1789 2

    Equat.    Gal    SGal    Ecl

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2020.12.05-01:17:23

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