The regions of formation of C IV resonance lines in β Persei

New IUE images of the close binary β Persei in the phase interval 0.6P-0.8P were analysed in order to confirm or rectify conclusions previously suggested concerning the region where C IV lines are formed. Based on IUE observations taken with high dispersion and small aperture, Sahade and Hernández (...

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Autores principales: Brandi, Estela, García, Lía Guillermina, Kondo, Y., Sahade, Jorge
Formato: Articulo Comunicacion
Lenguaje:Inglés
Publicado: 1987
Materias:
Astronomía
Galaxia
bet per
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/141448
Aporte de:
SEDICI (UNLP) de Universidad Nacional de La Plata
id I19-R120-10915-141448
record_format dspace
institution Universidad Nacional de La Plata
institution_str I-19
repository_str R-120
collection SEDICI (UNLP)
language Inglés
topic Astronomía
Galaxia
bet per
spellingShingle Astronomía
Galaxia
bet per
Brandi, Estela
García, Lía Guillermina
Kondo, Y.
Sahade, Jorge
The regions of formation of C IV resonance lines in β Persei
topic_facet Astronomía
Galaxia
bet per
description New IUE images of the close binary β Persei in the phase interval 0.6P-0.8P were analysed in order to confirm or rectify conclusions previously suggested concerning the region where C IV lines are formed. Based on IUE observations taken with high dispersion and small aperture, Sahade and Hernández (1985) concluded that the resonance lines of Si IV would originate in regions near the B8 V component. Instead, the C IV behaviour of velocity-wise in phases 0.65P-0.78P would seem to suggest that this ion would form in a region of the extended envelope that surrounds the whole system. Our recent IUE images, taken with high dispersion and large aperture that cover precisely the phase interval that was not well covered with the first set of observations, show that, in fact, the C IV resonance doublet behaves in the same way as the Si IV. Therefore, Si IV and C IV are formed in the same region of the envelope that surrounds the B8 V component and there is not, indeed, evidence for the existence of more than one high temperature region in the system of Per, such as it had been thought on the basis of former material. On each spectrum the C IV lines are weaker than Si IV. As the available material is not homogeneous, we can not determine variations, with phase in the line profiles and intensities. A new set of observations covering all the orbital cycle ought to be secured to be able to explain the different behaviour of the intensities.
format Articulo
Comunicacion
author Brandi, Estela
García, Lía Guillermina
Kondo, Y.
Sahade, Jorge
author_facet Brandi, Estela
García, Lía Guillermina
Kondo, Y.
Sahade, Jorge
author_sort Brandi, Estela
title The regions of formation of C IV resonance lines in β Persei
title_short The regions of formation of C IV resonance lines in β Persei
title_full The regions of formation of C IV resonance lines in β Persei
title_fullStr The regions of formation of C IV resonance lines in β Persei
title_full_unstemmed The regions of formation of C IV resonance lines in β Persei
title_sort regions of formation of c iv resonance lines in β persei
publishDate 1987
url http://sedici.unlp.edu.ar/handle/10915/141448
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