Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 488, Issue 1, Pages 64-77Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stz1661
Keywords
binaries: close; stars: magnetic field; stars: massive; stars: oscillations
Categories
Funding
- Universite Grenoble Alpes
- Institut de Planetologie et d'Astrophysique de Grenoble (IPAG)
- Agence Nationale pour la Recherche [ANR-06-BLAN-0421, ANR-10-BLAN-0505, ANR-10-LABX56, ANR-11-LABX-13]
- Institut National des Sciences de l'Univers (INSU PNP)
- CEA-LETI based on CNES RT
- VIZIER data bases (CDS, Strasbourg, France)
- AFJM
- Natural Sciences and Engineering Research Council of Canada (NSERC)
- Annie Jump Cannon Fellowship
- University of Delaware
- Mount Cuba Astronomical Observatory [02/010/BKM18/0136]
- Austrian Fonds zur Forderung der wissenschaftlichen Forschung (FWF) [V431-NBL]
- Austrian Space Application Programme (ASAP) of the Austrian Research Promotion Agency (FFG)
- ERC through SPIRE [647383]
- CNES PLATO grant at CEA-Saclay
- NCN [2016/21/B/ST9/01126]
- Polish National Science Center (NCN) [2015/18/A/ST9/00578]
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epsilon Lupi A is a binary system consisting of two main-sequence early B-type stars Aa and Ab in a short period, moderately eccentric orbit. The close binary pair is the only doubly magnetic massive binary currently known. Using photometric data from the BRITE Constellation we identify a modest heartbeat variation. Combining the photometry with radial velocities of both components we determine a full orbital solution including empirical masses and radii. These results are compared with stellar evolution models as well as interferometry and the differences discussed. We also find additional photometric variability at several frequencies, finding it unlikely these frequencies can be caused by tidally excited oscillations. We do, however, determine that these signals are consistent with gravity mode pulsations typical for slowly pulsating B stars. Finally we discuss how the evolution of this system will be affected by magnetism, determining that tidal interactions will still be dominant.
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