Modelagem de Estrelas do Ramo Horizontal

Detalhes bibliográficos
Ano de defesa: 2019
Autor(a) principal: Martins, Radi melo
Orientador(a): Não Informado pela instituição
Banca de defesa: Não Informado pela instituição
Tipo de documento: Dissertação
Tipo de acesso: Acesso aberto
Idioma: por
Instituição de defesa: Universidade Cruzeiro do Sul
Brasil
Programa de Pós Graduação em Astrofísica e Física Computacional
Cruzeiro do Sul
Programa de Pós-Graduação: Não Informado pela instituição
Departamento: Não Informado pela instituição
País: Não Informado pela instituição
Palavras-chave em Português:
Link de acesso: https://repositorio.cruzeirodosul.edu.br/handle/123456789/4022
Resumo: The Horizontal Branch is a stage of stellar evolution that immediately follows the red giant branch in low mass stars. This phase is common in stellar systems, and, when present, the HB stars may lead to uncertainties in stellar population analysis of the spectra. This is because, although they are old stars, depending on the mass loss during the giant phase, they can reach very high temperatures in the HB, inducing a false identification of young population. Models of stellar population used in stellar population analysis of these systems generally do not take this into account. This, however, has been improving over the years. Thus, it is important to have available spectra representative of this phase, which can be used by the spectral synthesis codes to generate more realistic stellar population spectra. In this work we produced a library of theoretical stellar spectra with the main characteristics of the HB stars, both atmospheric and chemical, to be used by stellar population models. The library was created in the spectral range from 3000 to 7000 Å, with temperatures from 5000 K to 25000K, log (g) from 2.0 to 4.5 dex, for 5 different metallicity values and 4 different values of He abundance.