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Emission from stellar wind bubbles interacting with an extragalactic jet

Departament de Física Quàntica i Astrofísica, Institut de Ciències del Cosmos (ICC), Universitat de Barcelona (IEEC-UB), Martí i Franquès 1, E08028 Barcelona, Spain

E-mail Address: ntorresalba@icc.ub.edu

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and

V. Bosch-Ramon

Departament de Física Quàntica i Astrofísica, Institut de Ciències del Cosmos (ICC), Universitat de Barcelona (IEEC-UB), Martí i Franquès 1, E08028 Barcelona, Spain

E-mail Address: vbosch@fqa.ub.edu

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https://doi.org/10.1142/S0218271818440182Cited by:0 (Source: Crossref)

This article is part of the issue:

Special Issue — Selected Papers of HEPRO VI; Editors: F. Aharonian, G. S. Bisnovatyi-Kogan, S. G. Moiseenko and M. V. Glushikhina

Abstract

The inner regions of galaxies are rich in gas and stars that can interact with the jet and produce high-energy nonthermal emission, as well as significantly mass-load the jet. In this work, we focus on a population of stars with strong winds, which accumulate material around the star outside the jet, confined by pressure equilibrium with the environment, in the form of a bubble. When these bubbles reach the jet, a shock is produced in the external bubble layer, which may cause part of the material to be peeled away and carried upstream at the contact discontinuity (CD). Part of the remaining bubble may penetrate the jet, and eventually detach and accelerate up to relativistic speeds, producing nonthermal emission.

We conclude that, for the studied population, these events are unlikely to mass-load the jet significantly and affect it dynamically. Our results show that the generated emission is potentially detectable for nearby sources, though not as persistent radiation, but rather in the form of long “flares” lasting for a few years, and with an event rate of about a few per century.

Keywords:

PACS: 98.54, 98.62.Nx, 98.62.Lv

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