Formación de Estrellas de Neutrones por Explosiones de Supernova en Sistemas Binarios con un Agujero Negro
From the detection of gravitational wave sources GW200105 and GW200115, produced by the merging of a neutron star and a black hole, it took special relevance understanding how this kind of systems originates. One of the channels which explain the formation of this kind of binaries, is the isolated e...
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| Tipo de recurso: | tesis de maestría |
| Estado: | Versión aceptada para publicación |
| Fecha de publicación: | 2024 |
| País: | México |
| Institución: | Instituto Nacional de Astrofísica, Óptica y Electrónica |
| Repositorio: | Repositorio Institucional del INAOE |
| Idioma: | español |
| OAI Identifier: | oai:inaoe.repositorioinstitucional.mx:1009/2524 |
| Acceso en línea: | http://inaoe.repositorioinstitucional.mx/jspui/handle/1009/2524 |
| Access Level: | acceso abierto |
| Palabra clave: | info:eu-repo/classification/Neutron Star/Neutron Star info:eu-repo/classification/Black Hole/Black Hole info:eu-repo/classification/Supernova/Supernova info:eu-repo/classification/Smoothed-particle Hydrodynamics/Smoothed-particle Hydrodynamics info:eu-repo/classification/Binary System Neutron Star/Binary System Neutron Star info:eu-repo/classification/Binary System/Binary System info:eu-repo/classification/cti/1 info:eu-repo/classification/cti/21 info:eu-repo/classification/cti/2199 |
| Sumario: | From the detection of gravitational wave sources GW200105 and GW200115, produced by the merging of a neutron star and a black hole, it took special relevance understanding how this kind of systems originates. One of the channels which explain the formation of this kind of binaries, is the isolated evolution of binary systems with two massive stars, where both of remnants are born from a gravitational core collapse of their progenitor star at the ending of their evolutive stage. In this channel, the first remnant to be born is a black hole, since its progeni- tor is the more massive of the binary. Then, it takes place a failed supernova. Then, in a similar way, the companion star goes through a core collapse, after which it forms a proto-neutron star, and later it occurs a supernova. In this work we explore the stage related to this supernova, where a fraction of the matter released by the star will be recaptured by the neutron star’s gravitational field, increasing its mass, with the purpose of study the supernova’s effect on final individual masses and binary’s orbital properties. In the approach used in this work, both the black hole and the neutron star are supposed to interact with their environment only by Newtonian gravity, while magnetic fields and relativistic effects are not taken into account. For the supernova explosion we study two different cases. Firstly, we suppose the explosion has spherical symmetry, changing only the energy of the explosion. Then, we introduce an asymmetry in the explosion, which it will transfer momentum to the neutron star, known as natal kick, whose intensity deppends on the asymmetry degree and energy of the explosion. Using the results obtained from these simulations, we analyze the individual physical parameters of each member of the binary, such as accreted mass, mass accretion rate and spin. Then, we compute the orbital parameters of the binary system, such as eccentricity, semimajor axis, orbital period, effective spin and coalescence time of the resulting binary. |
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