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The single-sided pulsator CO Camelopardalis

Kurtz, D. W. and Handler, G. and Rappaport, S. A. and Saio, H. and Fuller, J. and Jacobs, T. and Schmitt, A. and Jones, D. and Vanderburg, A. and LaCourse, D. and Nelson, L. and Kahraman Aliçavuş, F. and Giarrusso, M. (2020) The single-sided pulsator CO Camelopardalis. Monthly Notices of the Royal Astronomical Society, 494 (4). pp. 5118-5133. ISSN 0035-8711. doi:10.1093/mnras/staa989.

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CO Cam (TIC 160268882) is the second ‘single-sided pulsator’ to be discovered. These are stars where one hemisphere pulsates with a significantly higher amplitude than the other side of the star. CO Cam is a binary star comprised of an Am δ Sct primary star with T_(eff) = 7070 ± 150 K, and a spectroscopically undetected G main-sequence secondary star. The dominant pulsating side of the primary star is centred on the L₁ point. We have modelled the spectral energy distribution combined with radial velocities, and independently the TESS light curve combined with radial velocities. Both of these give excellent agreement and robust system parameters for both stars. The δ Sct star is an oblique pulsator with at least four low radial overtone (probably) f modes with the pulsation axis coinciding with the tidal axis of the star, the line of apsides. Preliminary theoretical modelling indicates that the modes must produce much larger flux perturbations near the L₁ point, although this is difficult to understand because the pulsating star does not come near to filling its Roche lobe. More detailed models of distorted pulsating stars should be developed. These newly discovered single-sided pulsators offer new opportunities for astrophysical inference from stars that are oblique pulsators in close binary stars.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Kurtz, D. W.0000-0002-1015-3268
Handler, G.0000-0001-7756-1568
Fuller, J.0000-0002-4544-0750
Jones, D.0000-0003-3947-5946
Vanderburg, A.0000-0001-7246-5438
Kahraman Aliçavuş, F.0000-0002-9036-7476
Giarrusso, M.0000-0002-4453-1597
Additional Information:© 2020 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 ( Accepted 2020 April 6. Received 2020 April 5; in original form 2020 February 14. Published: 13 April 2020. DWK acknowledges financial support from the UK Science and Technology Facilities Council (STFC) via grant ST/M000877/1. GH and FKA acknowledge financial support by the Polish National Science Centre (NCN) under grant 2015/18/A/ST9/00578, and thanks Elizaveta Kozlova for making the paper by Wojtkiewicz-Okulicz available. JF acknowledges support from an Innovator Grant from The Rose Hills Foundation, and the Sloan Foundation through grant FG-2018-10515. 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. LN thanks the Natural Sciences and Engineering Research Council (NSERC) of Canada for funding and thanks J. Aiken for his technical assistance. We thank Barry Smalley, Simon Murphy, and Daniel Holdsworth for useful suggestions and discussions, and we thank the anonymous referee for a thoughtful and useful report. We thank Richard Bischoff for supplying his team’s CO Cam spectra obtained with telescopes of the University Observatory Jena, which is operated by the Astrophysical Institute of the Friedrich-Schiller University. MG acknowledges financial support from the 5th National Committee of the Italian National Institute for Nuclear Physics (INFN) under the grant MAPS_3D. We thank Richard Bischoff for supplying his team’s CO Cam spectra. This paper includes data collected by the TESS mission. Funding for the TESS mission is provided by the NASA Explorer Program. Funding for the TESS Asteroseismic Science Operations Centre is provided by the Danish National Research Foundation (grant agreement no. DNRF106), ESA PRODEX (PEA 4000119301), and Stellar Astrophysics Centre (SAC) at Aarhus University.
Group:Astronomy Department
Funding AgencyGrant Number
Science and Technology Facilities Council (STFC)ST/M000877/1
National Science Centre (Poland)2015/18/A/ST9/00578
Rose Hills FoundationUNSPECIFIED
Alfred P. Sloan FoundationFG-2018-10515
European Regional Development FundAYA2017-83383-P
Ministerio de Ciencia e Innovación (MCINN)P/308614
Ministry of Economy, Industry, Trade and Knowledge (Canary Islands)UNSPECIFIED
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
Istituto Nazionale di Fisica Nucleare (INFN)MAPS_3D
Danish National Research FoundationDNRF106
European Space Agency (ESA)PEA 4000119301
Aarhus UniversityUNSPECIFIED
Subject Keywords:stars: individual: CO Cam (TIC 160268882; HD 106112) – stars: oscillations – stars: variables: δ Scuti
Issue or Number:4
Record Number:CaltechAUTHORS:20200519-122024701
Persistent URL:
Official Citation:D W Kurtz, G Handler, S A Rappaport, H Saio, J Fuller, T Jacobs, A Schmitt, D Jones, A Vanderburg, D LaCourse, L Nelson, F Kahraman Aliçavuş, M Giarrusso, The single-sided pulsator CO Camelopardalis, Monthly Notices of the Royal Astronomical Society, staa989,
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:103315
Deposited By: Tony Diaz
Deposited On:19 May 2020 19:51
Last Modified:16 Nov 2021 18:20

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