The Multiple Star 14 Aurigae.

The multiple star 14 Aurigae (= ADS 3824) contains five visual members, of which A and C (both of them single-lined spectroscopic binaries) form a physical system. Extreme ultraviolet observations reveal a hot white dwarf superposed on 14 Aur C. Ultraviolet spectroscopy reveals that it is a distant...

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Main Authors: Webbink, R. F., Etzel, P. B., Guinan, E. F., Holberg, J. B., Burleigh, M. R., Barstow, M. A., Sion, E. M.
Format: Villanova Faculty Authorship
Language:English
Published: 2001
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spelling The Multiple Star 14 Aurigae.
Webbink, R. F.
Etzel, P. B.
Guinan, E. F.
Holberg, J. B.
Burleigh, M. R.
Barstow, M. A.
Sion, E. M.
The multiple star 14 Aurigae (= ADS 3824) contains five visual members, of which A and C (both of them single-lined spectroscopic binaries) form a physical system. Extreme ultraviolet observations reveal a hot white dwarf superposed on 14 Aur C. Ultraviolet spectroscopy reveals that it is a distant companion to the optical spectroscopic binary, but that is a physical member of the system. Capitalizing on the fact that the visible component of 14 Aur A, KW Aur, is somewhat evolved, and is both an ellipsoidal variable and δ Scuti pulsator, we are able to model this quintuple system, obtaining both an evolutionary age for the system and a cooling age for the white dwarf, also masses for all five components, orbital inclinations for the two spectroscopic binaries, and an improved distance estimate to the system. Our results provide empirical values of the pulsation constants of KW Aur, and an estimate of the initial as well as final mass of the white dwarf.
2001
Villanova Faculty Authorship
vudl:176589
Astronomical Institute of the Academy of Sciences of the Czech Republic, 2001, 37-41.
en
dc.title_txt_mv The Multiple Star 14 Aurigae.
dc.creator_txt_mv Webbink, R. F.
Etzel, P. B.
Guinan, E. F.
Holberg, J. B.
Burleigh, M. R.
Barstow, M. A.
Sion, E. M.
dc.description_txt_mv The multiple star 14 Aurigae (= ADS 3824) contains five visual members, of which A and C (both of them single-lined spectroscopic binaries) form a physical system. Extreme ultraviolet observations reveal a hot white dwarf superposed on 14 Aur C. Ultraviolet spectroscopy reveals that it is a distant companion to the optical spectroscopic binary, but that is a physical member of the system. Capitalizing on the fact that the visible component of 14 Aur A, KW Aur, is somewhat evolved, and is both an ellipsoidal variable and δ Scuti pulsator, we are able to model this quintuple system, obtaining both an evolutionary age for the system and a cooling age for the white dwarf, also masses for all five components, orbital inclinations for the two spectroscopic binaries, and an improved distance estimate to the system. Our results provide empirical values of the pulsation constants of KW Aur, and an estimate of the initial as well as final mass of the white dwarf.
dc.date_txt_mv 2001
dc.format_txt_mv Villanova Faculty Authorship
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dc.source_txt_mv Astronomical Institute of the Academy of Sciences of the Czech Republic, 2001, 37-41.
dc.language_txt_mv en
author Webbink, R. F.
Etzel, P. B.
Guinan, E. F.
Holberg, J. B.
Burleigh, M. R.
Barstow, M. A.
Sion, E. M.
spellingShingle Webbink, R. F.
Etzel, P. B.
Guinan, E. F.
Holberg, J. B.
Burleigh, M. R.
Barstow, M. A.
Sion, E. M.
The Multiple Star 14 Aurigae.
author_facet Webbink, R. F.
Etzel, P. B.
Guinan, E. F.
Holberg, J. B.
Burleigh, M. R.
Barstow, M. A.
Sion, E. M.
dc_source_str_mv Astronomical Institute of the Academy of Sciences of the Czech Republic, 2001, 37-41.
format Villanova Faculty Authorship
author_sort Webbink, R. F.
dc_date_str 2001
dc_title_str The Multiple Star 14 Aurigae.
description The multiple star 14 Aurigae (= ADS 3824) contains five visual members, of which A and C (both of them single-lined spectroscopic binaries) form a physical system. Extreme ultraviolet observations reveal a hot white dwarf superposed on 14 Aur C. Ultraviolet spectroscopy reveals that it is a distant companion to the optical spectroscopic binary, but that is a physical member of the system. Capitalizing on the fact that the visible component of 14 Aur A, KW Aur, is somewhat evolved, and is both an ellipsoidal variable and δ Scuti pulsator, we are able to model this quintuple system, obtaining both an evolutionary age for the system and a cooling age for the white dwarf, also masses for all five components, orbital inclinations for the two spectroscopic binaries, and an improved distance estimate to the system. Our results provide empirical values of the pulsation constants of KW Aur, and an estimate of the initial as well as final mass of the white dwarf.
title The Multiple Star 14 Aurigae.
title_full The Multiple Star 14 Aurigae.
title_fullStr The Multiple Star 14 Aurigae.
title_full_unstemmed The Multiple Star 14 Aurigae.
title_short The Multiple Star 14 Aurigae.
title_sort multiple star 14 aurigae.
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language English
collection_title_sort_str multiple star 14 aurigae.
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