Chromospheric models of dwarf M stars

We present chromospheric models for two dM stars considered as "basal" stars due to the low level of chromospheric activity, and compare them with the model for a very active, flare star obtained in a previous paper. These models are not based on a single spectral feature, but on the conti...

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Autores principales: Mauas, P.J.D., Falchi, A., Pasquini, L., Pallavicini, R.
Formato: JOUR
Materias:
Stars: Atmospheres
Stars: Chromosphere
Stars: Late-type
Acceso en línea:http://hdl.handle.net/20.500.12110/paper_00046361_v326_n1_p249_Mauas
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id todo:paper_00046361_v326_n1_p249_Mauas
record_format dspace
spelling todo:paper_00046361_v326_n1_p249_Mauas2023-10-03T13:59:49Z Chromospheric models of dwarf M stars Mauas, P.J.D. Falchi, A. Pasquini, L. Pallavicini, R. Stars: Atmospheres Stars: Chromosphere Stars: Late-type We present chromospheric models for two dM stars considered as "basal" stars due to the low level of chromospheric activity, and compare them with the model for a very active, flare star obtained in a previous paper. These models are not based on a single spectral feature, but on the continuum in a broad wavelength range (3500 - 9000 Å), on many line profiles corresponding to three different atoms (H, Ca, Na), and on the Mg II h and k flux. We show that a marked chromosphere is present even for stars with the lowest levels of activity, and that the active stars have both a chromospheric temperature rise at larger column mass and a higher chromospheric temperature. These characteristics are responsible for the presence of the Balmer lines in emission in the dMe stars. We also show that the additional energy required to transform a dM star into an active star must be deposited in the high chromosphere, just below the transition region. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_00046361_v326_n1_p249_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: Chromosphere
Stars: Late-type
spellingShingle Stars: Atmospheres
Stars: Chromosphere
Stars: Late-type
Mauas, P.J.D.
Falchi, A.
Pasquini, L.
Pallavicini, R.
Chromospheric models of dwarf M stars
topic_facet Stars: Atmospheres
Stars: Chromosphere
Stars: Late-type
description We present chromospheric models for two dM stars considered as "basal" stars due to the low level of chromospheric activity, and compare them with the model for a very active, flare star obtained in a previous paper. These models are not based on a single spectral feature, but on the continuum in a broad wavelength range (3500 - 9000 Å), on many line profiles corresponding to three different atoms (H, Ca, Na), and on the Mg II h and k flux. We show that a marked chromosphere is present even for stars with the lowest levels of activity, and that the active stars have both a chromospheric temperature rise at larger column mass and a higher chromospheric temperature. These characteristics are responsible for the presence of the Balmer lines in emission in the dMe stars. We also show that the additional energy required to transform a dM star into an active star must be deposited in the high chromosphere, just below the transition region.
format JOUR
author Mauas, P.J.D.
Falchi, A.
Pasquini, L.
Pallavicini, R.
author_facet Mauas, P.J.D.
Falchi, A.
Pasquini, L.
Pallavicini, R.
author_sort Mauas, P.J.D.
title Chromospheric models of dwarf M stars
title_short Chromospheric models of dwarf M stars
title_full Chromospheric models of dwarf M stars
title_fullStr Chromospheric models of dwarf M stars
title_full_unstemmed Chromospheric models of dwarf M stars
title_sort chromospheric models of dwarf m stars
url http://hdl.handle.net/20.500.12110/paper_00046361_v326_n1_p249_Mauas
work_keys_str_mv AT mauaspjd chromosphericmodelsofdwarfmstars
AT falchia chromosphericmodelsofdwarfmstars
AT pasquinil chromosphericmodelsofdwarfmstars
AT pallavicinir chromosphericmodelsofdwarfmstars
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