Detalles de publicación
PP 017043
Triple system HD 201433 with a SPB star component seen by BRITE-Constellation: Pulsation, differential rotation, and angular momentum transfer
1 Institute for Astrophysics, University of Vienna, Türkenschanzstrasse 17, 1180 Vienna, Austria
2 Laboratoire AIM, CEA/DRF CNRS - Université Denis Diderot IRFU/SAp, 91191 Gif-sur-Yvette Cedex, France
3 Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain
4 Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain
5 Instytut Astronomiczny, Uniwersytet Wrocławski, Kopernika 11, 51-622 Wrocław, Poland
6 Institut für Kommunnikationsnetze und Satellitenkommunikation, Technical University Graz, Inffeldgasse 12, 8010 Graz, Austria
7 Instituut voor Sterrenkunde, K.U. Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
8 Institute of Astronomy, Russian Academy of Sciences, Pyatnitskaya 48, 119017 Moscow, Russia
9 Special Astrophysical Observatory, Russian Academy of Sciences, 369167, Nizhnii Arkhyz, Russia
10 Nicolaus Copernicus Astronomical Center, ul. Bartycka 18, 00-716 Warsaw, Poland
11 Department of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T1Z1, Canada
12 Département de physique and Centre de Recherche en Astrophysique du Québec (CRAQ), Université de Montréal, CP 6128, Succ.
Centre-Ville, Montréal, Québec, H3C 3J7, Canada
13 Institute of Automatic Control, Silesian University of Technology, Akademicka 16, 44-100 Gliwice, Poland
14 Department of Astronomy & Astrophysics, University of Toronto, 50 St. George Street, Toronto, Ontario, M5S 3H4, Canada
15 Department of Physics, Royal Military College of Canada, PO Box 17000, Station Forces, Kingston, Ontario, K7K 7B4, Canada
16 Institut für Astro- und Teilchenphysik, Universität Innsbruck, Technikerstrasse 25/8, 6020 Innsbruck, Austria
Context. Stellar rotation affects the transport of chemical elements and angular momentum and is therefore a key process during
stellar evolution, which is still not fully understood. This is especially true for massive OB-type stars, which are important for the
chemical enrichment of the universe. It is therefore important to constrain the physical parameters and internal angular momentum
distribution of massive OB-type stars to calibrate stellar structure and evolution models. Stellar internal rotation can be probed through
asteroseismic studies of rotationally split non radial oscillations but such results are still quite rare, especially for stars more massive
than the Sun. The slowly pulsating B9V star HD201433 is known to be part of a single-lined spectroscopic triple system, with two
low-mass companions orbiting with periods of about 3.3 and 154 days.
Aims. Our goal is to measure the internal rotation profile of HD201433 and investigate the tidal interaction with the close companion.
Methods. We used probabilistic methods to analyse the BRITE- Constellation photometry and radial velocity measurements, to
identify a representative stellar model, and to determine the internal rotation profile of the star.
Results. Our results are based on photometric observations made by BRITE- Constellation and the Solar Mass Ejection Imager on
board the Coriolis satellite, high-resolution spectroscopy, and more than 96 years of radial velocity measurements. We identify a
sequence of nine frequency doublets in the photometric time series, consistent with rotationally split dipole modes with a period
spacing of about 5030 s. We establish that HD201433 is in principle a solid-body rotator with a very slow rotation period of 297±76
days. Tidal interaction with the inner companion has, however, significantly accelerated the spin of the surface layers by a factor
of approximately one hundred. The angular momentum transfer onto the surface of HD201433 is also reflected by the statistically
significant decrease of the orbital period of about 0.9 s during the last 96 years.
Conclusions. Combining the asteroseismic inferences with the spectroscopic measurements and the orbital analysis of the inner
binary system, we conclude that tidal interactions between the central SPB star and its inner companion have almost circularised the
orbit. They have, however, not yet aligned all spins of the system and have just begun to synchronise rotation.
stellar evolution, which is still not fully understood. This is especially true for massive OB-type stars, which are important for the
chemical enrichment of the universe. It is therefore important to constrain the physical parameters and internal angular momentum
distribution of massive OB-type stars to calibrate stellar structure and evolution models. Stellar internal rotation can be probed through
asteroseismic studies of rotationally split non radial oscillations but such results are still quite rare, especially for stars more massive
than the Sun. The slowly pulsating B9V star HD201433 is known to be part of a single-lined spectroscopic triple system, with two
low-mass companions orbiting with periods of about 3.3 and 154 days.
Aims. Our goal is to measure the internal rotation profile of HD201433 and investigate the tidal interaction with the close companion.
Methods. We used probabilistic methods to analyse the BRITE- Constellation photometry and radial velocity measurements, to
identify a representative stellar model, and to determine the internal rotation profile of the star.
Results. Our results are based on photometric observations made by BRITE- Constellation and the Solar Mass Ejection Imager on
board the Coriolis satellite, high-resolution spectroscopy, and more than 96 years of radial velocity measurements. We identify a
sequence of nine frequency doublets in the photometric time series, consistent with rotationally split dipole modes with a period
spacing of about 5030 s. We establish that HD201433 is in principle a solid-body rotator with a very slow rotation period of 297±76
days. Tidal interaction with the inner companion has, however, significantly accelerated the spin of the surface layers by a factor
of approximately one hundred. The angular momentum transfer onto the surface of HD201433 is also reflected by the statistically
significant decrease of the orbital period of about 0.9 s during the last 96 years.
Conclusions. Combining the asteroseismic inferences with the spectroscopic measurements and the orbital analysis of the inner
binary system, we conclude that tidal interactions between the central SPB star and its inner companion have almost circularised the
orbit. They have, however, not yet aligned all spins of the system and have just begun to synchronise rotation.