Equatorial outflows driven by jets in Population III microquasars

Binary systems of Population III can evolve to microquasars when one of the stars collapses into a black hole. When the compact object accretes matter at a rate greater than the Eddington rate, powerful jets and winds driven by strong radiation pressure should form. We investigate the structure of t...

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Detalles Bibliográficos
Autores principales:	Sotomayor Checa, Pablo Omar, Romero, Gustavo Esteban, Bosch-Ramon, Valentí
Formato:	Articulo Preprint
Lenguaje:	Inglés
Publicado:	2021
Materias:	Ciencias Astronómicas Accretion, accretion disks Stars: black holes Stars: winds, outflows Stars: Population III X-rays: binaries
Acceso en línea:	http://sedici.unlp.edu.ar/handle/10915/129283
Aporte de:	SEDICI (UNLP) de Universidad Nacional de La Plata

id	I19-R120-10915-129283
record_format	dspace
institution	Universidad Nacional de La Plata
institution_str	I-19
repository_str	R-120
collection	SEDICI (UNLP)
language	Inglés
topic	Ciencias Astronómicas Accretion, accretion disks Stars: black holes Stars: winds, outflows Stars: Population III X-rays: binaries
spellingShingle	Ciencias Astronómicas Accretion, accretion disks Stars: black holes Stars: winds, outflows Stars: Population III X-rays: binaries Sotomayor Checa, Pablo Omar Romero, Gustavo Esteban Bosch-Ramon, Valentí Equatorial outflows driven by jets in Population III microquasars
topic_facet	Ciencias Astronómicas Accretion, accretion disks Stars: black holes Stars: winds, outflows Stars: Population III X-rays: binaries
description	Binary systems of Population III can evolve to microquasars when one of the stars collapses into a black hole. When the compact object accretes matter at a rate greater than the Eddington rate, powerful jets and winds driven by strong radiation pressure should form. We investigate the structure of the jet-wind system for a model of Population III microquasar on scales beyond the jet-wind formation region. Using relativistic hydrodynamic simulations we find that the ratio of kinetic power between the jet and the disk wind determines the configuration of the system. When the power is dominated by the wind, the jet fills a narrow channel, collimated by the dense outflow. When the jet dominates the power of the system, part of its energy is diverted turning the wind into a quasi-equatorial flow, while the jet widens. From the results of our simulations, we implement semi-analytical calculations of the impact of the quasi-equatorial wind on scales of the order of the size of the binary system. Our results indicate that Population III microquasars might inject gamma rays and relativistic particles into the early intergalactic medium, contributing to its reionization at large distances from the binary system.
format	Articulo Preprint
author	Sotomayor Checa, Pablo Omar Romero, Gustavo Esteban Bosch-Ramon, Valentí
author_facet	Sotomayor Checa, Pablo Omar Romero, Gustavo Esteban Bosch-Ramon, Valentí
author_sort	Sotomayor Checa, Pablo Omar
title	Equatorial outflows driven by jets in Population III microquasars
title_short	Equatorial outflows driven by jets in Population III microquasars
title_full	Equatorial outflows driven by jets in Population III microquasars
title_fullStr	Equatorial outflows driven by jets in Population III microquasars
title_full_unstemmed	Equatorial outflows driven by jets in Population III microquasars
title_sort	equatorial outflows driven by jets in population iii microquasars
publishDate	2021
url	http://sedici.unlp.edu.ar/handle/10915/129283
work_keys_str_mv	AT sotomayorchecapabloomar equatorialoutflowsdrivenbyjetsinpopulationiiimicroquasars AT romerogustavoesteban equatorialoutflowsdrivenbyjetsinpopulationiiimicroquasars AT boschramonvalenti equatorialoutflowsdrivenbyjetsinpopulationiiimicroquasars
bdutipo_str	Repositorios
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Equatorial outflows driven by jets in Population III microquasars

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