Model for Population III microquasars

Checa, Pablo Sotomayor; Romero, Gustavo E.

doi:10.1051/0004-6361/201834191

Cited by 10 publications

(15 citation statements)

References 70 publications

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“…We have applied our study to PopIII MQs. In order to model the jet-wind interaction in these objects we have adopted the model developed by Sotomayor Checa and Romero (2019).…”

Section: Discussionmentioning

confidence: 99%

“…The wind provides an additional source of ultraviolet radiation and soft X-rays. Sotomayor Checa and Romero (2019) showed that in the context of Population III microquasars, the emission from disk wind may be higher than the blackbody emission from the disk.…”

Section: Super-critical Accretion Disks and Their Windsmentioning

confidence: 99%

“…4.1), although the mass, momentum, and energy dominance of the wind external regions leaves some freedom to set the value of this parameter. We have estimated the parameters of the disk using the model developed by Sotomayor Checa and Romero (2019). The disk is supposed to be in the optically-thick advectiondominated state with toroidal magnetic fields.…”

Section: Super-critical Accretion Disks and Their Windsmentioning

confidence: 99%

“…For instance, a narrow jet strongly collimated by a powerful wind may not be able to keep its integrity for long because of the growth of hydrodynamical instabilities. On the other hand, a broad jet and a quasi-equatorial wind could also lead to specific consequences because of the different impact on the ambient medium; note that jets in PopIII MQs are expected to play a role in the cosmic re-ionization after the formation of the first stars (Sotomayor Checa and Romero 2019).…”

Section: Introductionmentioning

confidence: 99%

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Equatorial outflows driven by jets in Population III microquasars

Checa

Romero

Bosch‐Ramon

2021

Astrophys Space Sci

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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.

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“…We have applied our study to PopIII MQs. In order to model the jet-wind interaction in these objects we have adopted the model developed by Sotomayor Checa and Romero (2019).…”

Section: Discussionmentioning

confidence: 99%

Section: Super-critical Accretion Disks and Their Windsmentioning

confidence: 99%

Section: Super-critical Accretion Disks and Their Windsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Equatorial outflows driven by jets in Population III microquasars

Checa

Romero

Bosch‐Ramon

2021

Astrophys Space Sci

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“…All calculations have been computed for a cosmological redshift value z = 10. Preliminary results have been presented in Romero & Sotomayor Checa (2018) and Sotomayor Checa & Romero (2019).…”

Section: Introductionmentioning

confidence: 99%

A model for microquasars of Population III

Checa,

Romero

2019

Preprint

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Context. Current simulations indicate that the first stars were formed predominantly in binary systems. The study of the contribution of the first accreting binary systems to the reionization and heating of the intergalactic medium requires the formulation of a concrete model for microquasars of Population III. Aims. We aim at constructing a complete model for microquasars where the donor star is of Population III. Methods. We consider that the mas-loss of the star is caused exclusively by the spill of matter through the Roche lobe towards the black hole. We calculate the spectral energy distribution of the radiation produced by the accretion disk, the radiation-pressure driven wind, and the relativistic particles in the jets, within the framework of a lepto-hadronic model. In addition, we estimate the impact on the reionization by the first microquasars. Results. We determine that Population III microquasars are powerful sources of ultraviolet radiation produced by the winds of their super-critical disks, and generate a broadband non-thermal emission in jets. Conclusions. Our results indicate that microquasars in the early Universe could have been important for the reionization and heating of the intergalactic medium.

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