2013A&A...560A..79L


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.11CEST19:31:08

2013A&A...560A..79L - Astronomy and Astrophysics, volume 560A, 79-79 (2013/12-1)

Simulating gamma-ray binaries with a relativistic extension of RAMSES.

LAMBERTS A., FROMANG S., DUBUS G. and TEYSSIER R.

Abstract (from CDS):

Gamma-ray binaries are composed of a massive star and a rotation-powered pulsar with a highly relativistic wind. The collision between the winds from both objects creates a shock structure where particles are accelerated, which results in the observed high-energy emission. We want to understand the impact of the relativistic nature of the pulsar wind on the structure and stability of the colliding wind region and highlight the differences with colliding winds from massive stars. We focus on how the structure evolves with increasing values of the Lorentz factor of the pulsar wind, keeping in mind that current simulations are unable to reach the expected values of pulsar wind Lorentz factors by orders of magnitude. We use high-resolution numerical simulations with a relativistic extension to the hydrodynamics code RAMSES we have developed. We perform two-dimensional simulations, and focus on the region close to the binary, where orbital motion can be neglected. We model different values of the Lorentz factor of the pulsar wind, up to 16. We determine analytic scaling relations between stellar wind collisions and gamma-ray binaries. They provide the position of the contact discontinuity. The position of the shocks strongly depends on the Lorentz factor. We find that the relativistic wind is more collimated than expected based on non-relativistic simulations. Beyond a certain distance, the shocked flow is accelerated to its initial velocity and follows adiabatic expansion. Finally, we provide guidance for extrapolation towards more realistic values of the Lorentz factor of the pulsar wind. We extended the adaptive mesh refinement code RAMSES to relativistic hydrodynamics. This code is suited to studying astrophysical objects, such as pulsar wind nebulae, gamma-ray bursts, or relativistic jets, and will be part of the next public release of RAMSES. Using this code we performed simulations of gamma-ray binaries up to Γp=16 and highlighted the limits and possibilities of current hydrodynamical models of gamma-ray binaries.

Abstract Copyright:

Journal keyword(s): hydrodynamics - relativistic processes - methods: numerical - X-rays: binaries - gamma rays: stars

Simbad objects: 5

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Number of rows : 5

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 761 2
2 HD 259440 HXB 06 32 59.2566624297 +05 48 01.162565528 9.17 9.58 9.12     B0pe 186 0
3 3FHL J1018.8-5857 HXB 10 19 02.270 -58 56 29.87           ~ 92 0
4 CPD-63 2495 HXB 13 02 47.6541729595 -63 50 08.625922862 10.34 10.72 9.98 10.03   O9.5Ve 674 1
5 V* V479 Sct HXB 18 26 15.0561532140 -14 50 54.249464136 12.02 12.23 11.27 11.04   ON6V((f))z 492 2

    Equat.    Gal    SGal    Ecl

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2020.07.11-19:31:08

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