Solar prominences line profiles

A numerical code to calculate the line profiles for different elements present in the solar atmosphere was developed for the particular case of solar prominences. The objective is to compare the calculated with the observed profiles in order to limit the range of variation of the physical parameters...

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Detalles Bibliográficos
Autores principales: Stenborg, G., Mauas, P., Rovira, M.
Formato: Articulo Comunicacion
Lenguaje:Español
Publicado: 1994
Materias:
Astronomía
Galaxia
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/155120
Aporte de:
SEDICI (UNLP) de Universidad Nacional de La Plata
id I19-R120-10915-155120
record_format dspace
spelling I19-R120-10915-1551202023-07-06T20:02:03Z http://sedici.unlp.edu.ar/handle/10915/155120 issn:1669-9521 Solar prominences line profiles Stenborg, G. Mauas, P. Rovira, M. 1994 2023-07-06T11:34:37Z es Astronomía Galaxia A numerical code to calculate the line profiles for different elements present in the solar atmosphere was developed for the particular case of solar prominences. The objective is to compare the calculated with the observed profiles in order to limit the range of variation of the physical parameters, as temperature, pressure, electronic density, total density and turbulence velocity, which characterize these phenomena. Asociación Argentina de Astronomía Articulo Comunicacion http://creativecommons.org/licenses/by-nc-sa/4.0/ Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) application/pdf
institution Universidad Nacional de La Plata
institution_str I-19
repository_str R-120
collection SEDICI (UNLP)
language Español
topic Astronomía
Galaxia
spellingShingle Astronomía
Galaxia
Stenborg, G.
Mauas, P.
Rovira, M.
Solar prominences line profiles
topic_facet Astronomía
Galaxia
description A numerical code to calculate the line profiles for different elements present in the solar atmosphere was developed for the particular case of solar prominences. The objective is to compare the calculated with the observed profiles in order to limit the range of variation of the physical parameters, as temperature, pressure, electronic density, total density and turbulence velocity, which characterize these phenomena.
format Articulo
Comunicacion
author Stenborg, G.
Mauas, P.
Rovira, M.
author_facet Stenborg, G.
Mauas, P.
Rovira, M.
author_sort Stenborg, G.
title Solar prominences line profiles
title_short Solar prominences line profiles
title_full Solar prominences line profiles
title_fullStr Solar prominences line profiles
title_full_unstemmed Solar prominences line profiles
title_sort solar prominences line profiles
publishDate 1994
url http://sedici.unlp.edu.ar/handle/10915/155120
work_keys_str_mv AT stenborgg solarprominenceslineprofiles
AT mauasp solarprominenceslineprofiles
AT roviram solarprominenceslineprofiles
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