Modelagem de Estrelas do Ramo Horizontal

• Ano de defesa: 2019
• Autor(a) principal: Martins, Radi melo
• 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
• Palavras-chave em Português: Ramo Horizontal; Populações estelares; Bibliotecas Bstelares; Modelos de atmosfera; CNPQ::CIENCIAS EXATAS E DA TERRA::ASTRONOMIA
• Link de acesso: https://repositorio.cruzeirodosul.edu.br/handle/123456789/4022

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.