Building reliable models of M dwarf chromospheres: The spectral diagnostics

As part of an ongoing project to study how reliable are the chromospheric models constructed semi-empirically to fit the chromospheric spectrum of cold stars, in this paper we study how changes in the assumed chromospheric structure of dM and dMe stars affect the emitted spectrum. In this way, we st...

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Guardado en:
Detalles Bibliográficos
Publicado: 2000
Materias:
Stars: atmospheres
Stars: chromospheres
Stars: late-type
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v539_n2PART1_p858_Mauas
http://hdl.handle.net/20.500.12110/paper_0004637X_v539_n2PART1_p858_Mauas
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_0004637X_v539_n2PART1_p858_Mauas
record_format dspace
spelling paper:paper_0004637X_v539_n2PART1_p858_Mauas2023-06-08T14:28:42Z Building reliable models of M dwarf chromospheres: The spectral diagnostics Stars: atmospheres Stars: chromospheres Stars: late-type As part of an ongoing project to study how reliable are the chromospheric models constructed semi-empirically to fit the chromospheric spectrum of cold stars, in this paper we study how changes in the assumed chromospheric structure of dM and dMe stars affect the emitted spectrum. In this way, we study if a given set of features can wholly determine the atmospheric structure, how large are the indeterminations in the atmospheric parameters deduced, and to what extent the atmospheric model computed can be considered unique. We find that the profiles of the Ca II K line or the Na D lines can be used to determine the structure of the Tmin region and that the Ha profile can provide good information on the structure of the chromosphere. The Lyα flux, in turn, can be used to constrain the position of the transition region. 2000 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v539_n2PART1_p858_Mauas http://hdl.handle.net/20.500.12110/paper_0004637X_v539_n2PART1_p858_Mauas
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic Stars: atmospheres
Stars: chromospheres
Stars: late-type
spellingShingle Stars: atmospheres
Stars: chromospheres
Stars: late-type
Building reliable models of M dwarf chromospheres: The spectral diagnostics
topic_facet Stars: atmospheres
Stars: chromospheres
Stars: late-type
description As part of an ongoing project to study how reliable are the chromospheric models constructed semi-empirically to fit the chromospheric spectrum of cold stars, in this paper we study how changes in the assumed chromospheric structure of dM and dMe stars affect the emitted spectrum. In this way, we study if a given set of features can wholly determine the atmospheric structure, how large are the indeterminations in the atmospheric parameters deduced, and to what extent the atmospheric model computed can be considered unique. We find that the profiles of the Ca II K line or the Na D lines can be used to determine the structure of the Tmin region and that the Ha profile can provide good information on the structure of the chromosphere. The Lyα flux, in turn, can be used to constrain the position of the transition region.
title Building reliable models of M dwarf chromospheres: The spectral diagnostics
title_short Building reliable models of M dwarf chromospheres: The spectral diagnostics
title_full Building reliable models of M dwarf chromospheres: The spectral diagnostics
title_fullStr Building reliable models of M dwarf chromospheres: The spectral diagnostics
title_full_unstemmed Building reliable models of M dwarf chromospheres: The spectral diagnostics
title_sort building reliable models of m dwarf chromospheres: the spectral diagnostics
publishDate 2000
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v539_n2PART1_p858_Mauas
http://hdl.handle.net/20.500.12110/paper_0004637X_v539_n2PART1_p858_Mauas
_version_ 1768542916081352704

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