A tidally tilted sectoral dipole pulsation mode in the eclipsing binary TIC 63328020

Creators: Rappaport, S. A.; Kurtz, D. W.; Handler, G.; Jones, D.; Nelson, L. A.; Saio, H.; Fuller, J.; Holdsworth, D.L.; Vanderburg, A.; Zak, J.; Skarka, M.; Aiken, J.; Maxted, P.F. L.; Stevens, D. J.; Feliz, D. l.; Kahraman Aliçavuş, F.

Abstract

We report the discovery of the third tidally tilted pulsator, TIC 63328020. Observations with the TESS satellite reveal binary eclipses with an orbital period of 1.1057 d, and δ Scuti-type pulsations with a mode frequency of 21.09533 d⁻¹. This pulsation exhibits a septuplet of orbital sidelobes as well as a harmonic quintuplet. Using the oblique pulsator model, the primary oscillation is identified as a sectoral dipole mode with l = 1, |m| = 1. We find the pulsating star to have M₁≃2.5M⊙⁠, R₁≃3R⊙⁠, and T_(eff, 1) ≃ 8000 K, while the secondary has M₂≃1.1M⊙⁠, R₂≃2R⊙⁠, and T_(eff, 2) ≃ 5600 K. Both stars appear to be close to filling their respective Roche lobes. The properties of this binary as well as the tidally tilted pulsations differ from the previous two tidally tilted pulsators, HD74423 and CO Cam, in important ways. We also study the prior history of this system with binary evolution models and conclude that extensive mass transfer has occurred from the current secondary to the primary.

Additional Information

© 2021 The Author(s). Published by Oxford University Press on behalf of 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 2021 January 27. Received 2021 January 14; in original form 2020 August 26. Published: 09 February 2021. We are grateful to an anonymous referee whose comments and suggestions helped clarify the presentations in this paper. This paper includes data collected by the TESS mission. Funding for the TESS mission is provided by the NASA Science Mission directorate. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. Based on observations made with the Isaac Newton Telescope operated by the Isaac Newton Group of Telescopes, which resides on the island of La Palma at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias. The authors thankfully acknowledge the technical expertise and assistance provided by the Spanish Supercomputing Network (Red Española de Supercomputación), as well as the computer resources used: the LaPalma Supercomputer, located at the Instituto de Astrofísica de Canarias. GH acknowledges financial support from the Polish National Science Center (NCN), grant no. 2015/18/A/ST9/00578. DJ acknowledges support from the State Research Agency (AEI) of the Spanish Ministry of Science, Innovation and Universities (MCIU) and the European Regional Development Fund (FEDER) under grant AYA2017-83383-P. DJ also acknowledges support under grant P/308614 financed by funds transferred from the Spanish Ministry of Science, Innovation and Universities, charged to the General State Budgets and with funds transferred from the General Budgets of the Autonomous Community of the Canary Islands by the Ministry of Economy, Industry, Trade and Knowledge. This research was supported by the Erasmus + programme of the European Union under grant no. 2017-1-CZ01-KA203-035562. LN thanks the Natural Sciences and Engineering Research Council of Canada for financial support through the Discovery Grants program. Some computations were carried out on the supercomputers managed by Calcul Québec and Compute Canada. The operation of these supercomputers is funded by the Canada Foundation for Innovation (CFI), NanoQuébec, Réseau de Médecine Génétique Appliquée, and the Fonds de recherche du Québec – Nature et technologies (FRQNT). JA thanks NSERC (Canada) for an Undergraduate Student Research Award (USRA). DJS acknowledges funding support from the Eberly Research Fellowship from The Pennsylvania State University Eberly College of Science. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. MS acknowledges the financial support of the Operational Program Research, Development and Education – Project Postdoc@MUNI (No. CZ.02.2.69/0.0/0.0/16_027/0008360). This project utilized data from the Digital Access to a Sky Century@Harvard ('DASCH') project at Harvard that is partially supported from NSF grants AST-0407380, AST-0909073, and AST-1313370. This paper also makes use of the Wide Angle Search for Planets (WASP) data set as provided by the WASP consortium and services at the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program (DOI 10.26133/NEA9). This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France. The original description of the VizieR service was published in Ochsenbein et al. (2000). This project also makes use of data from the Kilodegree Extremely Little Telescope ('KELT') survey, including support from The Ohio State University, Vanderbilt University, and Lehigh University, along with the KELT follow-up collaboration. Data Availability: The TESS data used in this paper are available on MAST. All other data used are reported in tables within the paper. The MESA binary evolution 'inlists' are available on the MESA Marketplace: http://cococubed.asu.edu/mesa_market/inlists.html.

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