ϵ Lupi: measuring the heartbeat of a doubly magnetic massive binary with BRITE Constellation

Creators: Pablo, H.; Shultz, M.; Fuller, J.; Wade, G. A.; Paunzen, E.; Mathis, S.; Le Bouquin, J.-B.; Pigulski, A.; Handler, G.; Alecian, E.; Kuschnig, R.; Moffat, A. F. J.; Neiner, C.; Popowicz, A.; Rucinski, S.; Smolec, R.; Weiss, W.; Zwintz, K.; BinaMIcS Collaboration

Abstract

ϵ 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.

Additional Information

© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). Accepted 2019 June 11. Received 2019 June 11; in original form 2019 April 3. Published: 21 June 2019. Based in part on data collected by the BRITE Constellation satellite mission, designed, built, launched, operated, and supported by the Austrian Research Promotion Agency (FFG), the University of Vienna, the Technical University of Graz, the University of Innsbruck, the Canadian Space Agency (CSA), the University of Toronto Institute for Aerospace Studies (UTIAS), the Foundation for Polish Science, Technology (FNiTP MNiSW), National Science Centre (NCN). Based on observations obtained at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. PIONIER was developed by the Université Grenoble Alpes, the Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), the Agence Nationale pour la Recherche (ANR-06-BLAN-0421, ANR-10-BLAN-0505, ANR-10-LABX56, ANR-11-LABX-13), and the Institut National des Sciences de l'Univers (INSU PNP and PNPS), in collaboration with CEA-LETI based on CNES R&T funding. This research has made use of the Washington Double Star Catalog maintained by the U.S. Naval Observatory. This research has used the Aspro8 and SearchCal9 services (Jean-Marie Mariotti Center), of the SIMBAD and VIZIER data bases (CDS, Strasbourg, France) and of the Astrophysics Data System (NASA). AFJM, MS, and GAW acknowledge support from the Natural Sciences and Engineering Research Council of Canada (NSERC). MS acknowledges support from the Annie Jump Cannon Fellowship supported by the University of Delaware and endowed by the Mount Cuba Astronomical Observatory. APo was responsible for image processing and automation of photometric routines for the data registered by BRITE-nanosatellite constellation, and was supported by BKMN grant no. 02/010/BKM18/0136. KZ acknowledges support by the Austrian Fonds zur Förderung der wissenschaftlichen Forschung (FWF, project V431-NBL) and the Austrian Space Application Programme (ASAP) of the Austrian Research Promotion Agency (FFG). WW acknowledges support by the Austrian Space Application Programme (ASAP) of the Austrian Research Promotion Agency (FFG). SM acknowledges support by the ERC through SPIRE (grant no. 647383) and CNES PLATO grant at CEA-Saclay. APi acknowledges support from the NCN grant no. 2016/21/B/ST9/01126. GH acknowledges support by the Polish National Science Center (NCN), grant no. 2015/18/A/ST9/00578.

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