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Title: Impact of red giant/AGB winds on active galactic nucleus jet propagation

Abstract

Context. Dense stellar winds may mass-load the jets of active galactic nuclei, although it is unclear on what time and spatial scales the mixing takes place. Aims. Our aim is to study the first steps of the interaction between jets and stellar winds, and also the scales on which the stellar wind mixes with the jet and mass-loads it. Methods. We present a detailed 2D simulation – including thermal cooling – of a bubble formed by the wind of a star designed to study the initial stages of jet-star interaction. We also study the first interaction of the wind bubble with the jet using a 3D simulation in which the star enters the jet. Stability analysis is carried out for the shocked wind structure to evaluate the distances over which the jet-dragged wind, which forms a tail, can propagate without mixing with the jet flow. Results. The 2D simulations point to quick wind bubble expansion and fragmentation after about one bubble shock crossing time. Three-dimensional simulations and stability analysis point to local mixing in the case of strong perturbations and relatively low density ratios between the jet and the jet dragged-wind, and to a possibly more stable shocked wind structuremore » at the phase of maximum tail mass flux. Analytical estimates also indicate that very early stages of the star jet-penetration time may be also relevant for massloading. The combination of these and previous results from the literature suggests highly unstable interaction structures and efficient wind-jet flow mixing on the scale of the jet interaction height. Conclusions. The winds of stars with strong mass loss can efficiently mix with jets from active galactic nuclei. In addition, the initial wind bubble shocked by the jet leads to a transient, large interaction surface. The interaction between jets and stars can produce strong inhomogeneities within the jet. As mixing is expected to be effective on large scales, even individual asymptotic giant branch stars can significantly contribute to the mass-load of the jet and thus affect its dynamics. Shear layer mass-entrainment could be important. The interaction structure can be a source of significant non-thermal emission.« less

Authors:
 [1];  [2];  [3]
+ Show Author Affiliations
  1. Univ. de Valencia (Spain)
  2. Univ. de Barcelona (Spain)
  3. Purdue Univ., West Lafayette, IN (United States); Deutsches Elektronen-Synchrotron (DESY), Zeuthen (Germany); RIKEN, Saitama (Japan)
Publication Date:
Research Org.:
Purdue Univ., West Lafayette, IN (United States)
Sponsoring Org.:
USDOE Office of Science (SC)
OSTI Identifier:
1540107
Grant/Contract Number:  
SC0016369
Resource Type:
Accepted Manuscript
Journal Name:
Astronomy and Astrophysics
Additional Journal Information:
Journal Volume: 606; Journal ID: ISSN 0004-6361
Publisher:
EDP Sciences
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; Astronomy & Astrophysics

Citation Formats

Perucho, M., Bosch-Ramon, V., and Barkov, M. V.. Impact of red giant/AGB winds on active galactic nucleus jet propagation. United States: N. p., 2017. Web. doi:10.1051/0004-6361/201630117.
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Perucho, M., Bosch-Ramon, V., & Barkov, M. V.. Impact of red giant/AGB winds on active galactic nucleus jet propagation. United States. https://doi.org/10.1051/0004-6361/201630117
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Perucho, M., Bosch-Ramon, V., and Barkov, M. V.. Thu . "Impact of red giant/AGB winds on active galactic nucleus jet propagation". United States. https://doi.org/10.1051/0004-6361/201630117. https://www.osti.gov/servlets/purl/1540107.
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@article{osti_1540107,
title = {Impact of red giant/AGB winds on active galactic nucleus jet propagation},
author = {Perucho, M. and Bosch-Ramon, V. and Barkov, M. V.},
abstractNote = {Context. Dense stellar winds may mass-load the jets of active galactic nuclei, although it is unclear on what time and spatial scales the mixing takes place. Aims. Our aim is to study the first steps of the interaction between jets and stellar winds, and also the scales on which the stellar wind mixes with the jet and mass-loads it. Methods. We present a detailed 2D simulation – including thermal cooling – of a bubble formed by the wind of a star designed to study the initial stages of jet-star interaction. We also study the first interaction of the wind bubble with the jet using a 3D simulation in which the star enters the jet. Stability analysis is carried out for the shocked wind structure to evaluate the distances over which the jet-dragged wind, which forms a tail, can propagate without mixing with the jet flow. Results. The 2D simulations point to quick wind bubble expansion and fragmentation after about one bubble shock crossing time. Three-dimensional simulations and stability analysis point to local mixing in the case of strong perturbations and relatively low density ratios between the jet and the jet dragged-wind, and to a possibly more stable shocked wind structure at the phase of maximum tail mass flux. Analytical estimates also indicate that very early stages of the star jet-penetration time may be also relevant for massloading. The combination of these and previous results from the literature suggests highly unstable interaction structures and efficient wind-jet flow mixing on the scale of the jet interaction height. Conclusions. The winds of stars with strong mass loss can efficiently mix with jets from active galactic nuclei. In addition, the initial wind bubble shocked by the jet leads to a transient, large interaction surface. The interaction between jets and stars can produce strong inhomogeneities within the jet. As mixing is expected to be effective on large scales, even individual asymptotic giant branch stars can significantly contribute to the mass-load of the jet and thus affect its dynamics. Shear layer mass-entrainment could be important. The interaction structure can be a source of significant non-thermal emission.},
doi = {10.1051/0004-6361/201630117},
journal = {Astronomy and Astrophysics},
number = ,
volume = 606,
place = {United States},
year = {2017},
month = {10}
}
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https://doi.org/10.1051/0004-6361/201630117
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text, January 2017

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