White dwarfs in binaries and hierarchical triple systems as a test for mass transfer models and close binary formation mechanisms

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dc.contributor.advisorAdvisor: Zorotovic, Mónica
dc.contributor.advisorAdvisor: Schreiber, Matthias
dc.contributor.authorLagos Vilches, Felipe
dc.coverage.spatialValparaíso
dc.date.accessioned2025-04-07T15:34:43Z
dc.date.available2025-04-07T15:34:43Z
dc.date.issued2021
dc.description.abstractMost stars with masses above ≈ 1M8 will end their lives as white dwarfs. Given that a non negligible fraction of such stars are in binary or multiple star systems, the characteristics of some of these white dwarfs will are affected by interactions between its progenitor and a close companion. These interactions can continue after the formation of the white dwarf producing a large variety of interesting objects and astrophysical phenomena like cataclysmic variables, double white dwarf binaries, super soft X-ray sources or type Ia supernovae. Formation of white dwarfs affected by binary interactions, or its subsequent interaction with a close companion, can be also enhanced due to perturbations exerted by a third companion. Under certain conditions, inner binaries in triple systems are prone to experience long term changes in their eccentricities, allowing otherwise non-interacting binaries to experience tidal migration, mass trans- fer, common envelope evolution or even mergers/collisions. In addition, although it is generally assumed that the interacting companion is another star, recent studies indicate that planets can interact with their host star, survive the metamorphosis of the latter into a white dwarf and later potentially pollute its atmosphere with heavy elements. Therefore, white dwarfs that reside in binary and triple configurations provide invaluable astrophysical laboratories to study stellar and binary evolution, orbital dynamics, and planet formation/evolution. Despite remarkable progress made in the last forty years in modeling binary interactions and the secular dynamic evolution of triple systems, the physics behind several processes, in particular those involved in the former, is still not well under- stood. This is mainly due to the fact that most of the currently available modeling tools are based on analytical simplifications involving parameters that must be fit- ted through (extensive and detailed) observations. With the aim of reducing this gap in our knowledge, I present in this thesis three different cases in which binaries and hierarchical triple systems will allow to test and improve current models of binary interactions and to measure the impact of tertiary companions in the formation of tight binaries.
dc.facultadFacultad de Ciencias
dc.identifier.urihttps://repositoriobibliotecas.uv.cl/handle/uvscl/15621
dc.language.isoen
dc.publisherUniversidad de Valparaíso
dc.rights.urihttp://creativecommons.org/licenses/by-nc-sa/3.0/cl/
dc.subjectBINARIAS ECLIPSANTES
dc.subjectESTRELLAS ENANAS BLANCAS
dc.titleWhite dwarfs in binaries and hierarchical triple systems as a test for mass transfer models and close binary formation mechanisms
dc.typeTDOC
uv.catalogadorPJR CIEN
uv.colectionTesis
uv.departamentoFacultad de Ciencias, Instituto de Física y Astronomía
uv.notageneralDoctorado en Astrofísica. Universidad de Valparaíso. 2021.

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