On the nature of the LBV/WR eclipsing binary system HD 5980

On the nature of the LBV/WR eclipsing binary system HD 5980

HD 5980 is a multiple star system in the Small Magellanic Cloud that underwent a luminous blue variable-like eruption in 1993-1994. The erupting star (star A) forms part of a close eclipsing binary whose companion's (star B) Wolf-Rayet nature has recently been questioned. The data analyzed in this paper cover the period 1979-2002, and support the WNE classification of star B. The orbital phase-dependent variations of ultraviolet P Cygni absorption lines imply that the wind speed of star A is 1700-2200 km s-1 and that of star B is 2600-3100 km s-1. These allow an estimate of the wind-wind collision (WWC) shock cone geometry and line profiles from the WWC region. Given the assumed mass-loss rates, only a small fraction of the observed emission line profiles may originate in the WWC region. The star A+starB binary pair is likely the result of evolution with mass transfer and/or evolution with rapid rotation, and provides a magnificent opportunity for studying the processes that occur in massive multiple systems at the stages of stellar evolution just prior to the supernova event.

Saved in:
Bibliographic Details
Main Author: Koenigsberger,G.
Format: Digital revista
Language:English
Published: Universidad Nacional Autónoma de México, Instituto de Astronomía 2004
Online Access:http://www.scielo.org.mx/scielo.php?script=sci_arttext&pid=S0185-11012004000200001
Tags: Add Tag
No Tags, Be the first to tag this record!
id oai:scielo:S0185-11012004000200001
record_format ojs
spelling oai:scielo:S0185-110120040002000012016-09-12On the nature of the LBV/WR eclipsing binary system HD 5980Koenigsberger,G. Stars/Binaries (Eclipsing) Stars/Individual (HD 5980) Stars/Winds Stars/Outflows Stars/Wolf-Rayet Stars/Variables (Luminous Blue Variables) HD 5980 is a multiple star system in the Small Magellanic Cloud that underwent a luminous blue variable-like eruption in 1993-1994. The erupting star (star A) forms part of a close eclipsing binary whose companion's (star B) Wolf-Rayet nature has recently been questioned. The data analyzed in this paper cover the period 1979-2002, and support the WNE classification of star B. The orbital phase-dependent variations of ultraviolet P Cygni absorption lines imply that the wind speed of star A is 1700-2200 km s-1 and that of star B is 2600-3100 km s-1. These allow an estimate of the wind-wind collision (WWC) shock cone geometry and line profiles from the WWC region. Given the assumed mass-loss rates, only a small fraction of the observed emission line profiles may originate in the WWC region. The star A+starB binary pair is likely the result of evolution with mass transfer and/or evolution with rapid rotation, and provides a magnificent opportunity for studying the processes that occur in massive multiple systems at the stages of stellar evolution just prior to the supernova event.info:eu-repo/semantics/openAccessUniversidad Nacional Autónoma de México, Instituto de AstronomíaRevista mexicana de astronomía y astrofísica v.40 n.2 20042004-01-01info:eu-repo/semantics/articletext/htmlhttp://www.scielo.org.mx/scielo.php?script=sci_arttext&pid=S0185-11012004000200001en
institution SCIELO
collection OJS
country México
countrycode MX
component Revista
access En linea
databasecode rev-scielo-mx
tag revista
region America del Norte
libraryname SciELO
language English
format Digital
author Koenigsberger,G.
spellingShingle Koenigsberger,G.
On the nature of the LBV/WR eclipsing binary system HD 5980
author_facet Koenigsberger,G.
author_sort Koenigsberger,G.
title On the nature of the LBV/WR eclipsing binary system HD 5980
title_short On the nature of the LBV/WR eclipsing binary system HD 5980
title_full On the nature of the LBV/WR eclipsing binary system HD 5980
title_fullStr On the nature of the LBV/WR eclipsing binary system HD 5980
title_full_unstemmed On the nature of the LBV/WR eclipsing binary system HD 5980
title_sort on the nature of the lbv/wr eclipsing binary system hd 5980
description HD 5980 is a multiple star system in the Small Magellanic Cloud that underwent a luminous blue variable-like eruption in 1993-1994. The erupting star (star A) forms part of a close eclipsing binary whose companion's (star B) Wolf-Rayet nature has recently been questioned. The data analyzed in this paper cover the period 1979-2002, and support the WNE classification of star B. The orbital phase-dependent variations of ultraviolet P Cygni absorption lines imply that the wind speed of star A is 1700-2200 km s-1 and that of star B is 2600-3100 km s-1. These allow an estimate of the wind-wind collision (WWC) shock cone geometry and line profiles from the WWC region. Given the assumed mass-loss rates, only a small fraction of the observed emission line profiles may originate in the WWC region. The star A+starB binary pair is likely the result of evolution with mass transfer and/or evolution with rapid rotation, and provides a magnificent opportunity for studying the processes that occur in massive multiple systems at the stages of stellar evolution just prior to the supernova event.
publisher Universidad Nacional Autónoma de México, Instituto de Astronomía
publishDate 2004
url http://www.scielo.org.mx/scielo.php?script=sci_arttext&pid=S0185-11012004000200001
work_keys_str_mv AT koenigsbergerg onthenatureofthelbvwreclipsingbinarysystemhd5980
_version_ 1756220823634444288

Similar Items