Skip to Main content Skip to Navigation
Journal articles

High-energy Particle Transport in Three-dimensional Hydrodynamic Models of Colliding-wind Binaries

Abstract : Massive stars in binary systems (such as WR 140, WR 147, or η Carinae) have long been regarded as potential sources of high-energy γ-rays. The emission is thought to arise in the region where the stellar winds collide and produce relativistic particles that subsequently might be able to emit γ-rays. Detailed numerical hydrodynamic simulations have already offered insight into the complex dynamics of the wind collision region (WCR), while independent analytical studies, albeit with simplified descriptions of the WCR, have shed light on the spectra of charged particles. In this paper, we describe a combination of these two approaches. We present a three-dimensional hydrodynamical model for colliding stellar winds and compute spectral energy distributions of relativistic particles for the resulting structure of the WCR. The hydrodynamic part of our model incorporates the line-driven acceleration of the winds, gravity, orbital motion, and the radiative cooling of the shocked plasma. In our treatment of charged particles, we consider diffusive shock acceleration in the WCR and the subsequent cooling via inverse Compton losses (including Klein-Nishina effects), bremsstrahlung, collisions, and other energy loss mechanisms.
Document type :
Journal articles
Complete list of metadata

https://hal-insu.archives-ouvertes.fr/insu-03618605
Contributor : Nathalie POTHIER Connect in order to contact the contributor
Submitted on : Thursday, March 24, 2022 - 2:13:27 PM
Last modification on : Friday, March 25, 2022 - 4:03:18 AM

Links full text

Identifiers

Collections

Citation

K. Reitberger, R. Kissmann, A. Reimer, O. Reimer, G. Dubus. High-energy Particle Transport in Three-dimensional Hydrodynamic Models of Colliding-wind Binaries. The Astrophysical Journal, 2014, 782, ⟨10.1088/0004-637X/782/2/96⟩. ⟨insu-03618605⟩

Share

Metrics

Record views

6