A window into δ Sct stellar interiors: understanding the eclipsing binary system TT Hor

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dc.contributor.authorStreamer, Margaret
dc.contributor.authorIreland, Michael
dc.contributor.authorMurphy, Simon
dc.contributor.authorBento, Joao
dc.date.accessioned2019-06-24T03:11:50Z
dc.date.available2019-06-24T03:11:50Z
dc.date.issued2018
dc.date.updated2022-07-31T08:19:16Z
dc.description.abstractThe semi-detached eclipsing binary system TT Hor has a δ Sct primary component (accretor) accreting mass from the secondary star (donor). We fit an eclipsing binary model from V, B, and I photometry combined with spectroscopy using PHOEBE. Radial velocity variations of the centre of mass of TT Hor AB over two years suggest the presence of a wide companion, consistent with a Kozai–Lidov resonance formation process for TT Hor AB. Evolutionary models computed with MESA give the initial mass of the donor as ≈1.6 M⊙ and that of the accretor as ≈1.3 M⊙. The initial binary orbit has a similar initial separation to the currently observed separation of 11.4 R⊙. Mass transfer commences at an age of 2.5 Gyr when the donor is a subgiant. We model the accretor as a tidally locked 2.2 ± 0.2 M⊙ δ Sct pulsator which has accreted ≈0.9 M⊙ of slightly He-enriched material (mean ΔY < 0.01) from the donor over the last 90 Myr. The best fit from all measured parameters and evolutionary states is for a system metallicity of [M/H] = 0.15. A pulsation model of the primary gives a self-consistent set of modes. Our observed oscillation frequencies match to within 0.3 per cent and the system parameters within uncertainties. However, we cannot claim that our identified modes are definitive, and suggest follow-up time-series spectroscopy at high resolution in order to verify our identified modes. With the higher signal-to-noise ratio and continuous observations with TESS, more reliable mode identification due to frequency and amplitude changes during the eclipse is likely.
dc.description.sponsorshipThis research (MS) is supported by an Australian Government Research Training Program (RTP) Scholarship. SJM is the recipient of an Australian Research Council Discovery Early Career Award (project number 180101104), funded by the Australian Governmenten_AU
dc.format.mimetypeapplication/pdfen_AU
dc.identifier.issn0035-8711en_AU
dc.identifier.urihttp://hdl.handle.net/1885/164168
dc.language.isoen_AUen_AU
dc.provenancehttp://sherpa.ac.uk/romeo/issn/0035-8711/..."author can archive publisher's version/PDF" from SHERPA/RoMEO site (as at 24/06/19). This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.en_AU
dc.publisherWiley
dc.relationhttp://purl.org/au-research/grants/arc/DE180101104
dc.rights© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society
dc.sourceMonthly Notices of the Royal Astronomical Society
dc.titleA window into δ Sct stellar interiors: understanding the eclipsing binary system TT Hor
dc.typeJournal article
dcterms.accessRightsOpen Accessen_AU
local.bibliographicCitation.issue1en_AU
local.bibliographicCitation.lastpage1383en_AU
local.bibliographicCitation.startpage1372en_AU
local.contributor.affiliationStreamer, Margaret, College of Science, ANUen_AU
local.contributor.affiliationIreland, Michael, College of Science, ANUen_AU
local.contributor.affiliationMurphy, Simon, The University of Sydneyen_AU
local.contributor.affiliationBento (Da Silva Bento), Joao, College of Science, ANUen_AU
local.contributor.authoremailu5544212@anu.edu.auen_AU
local.contributor.authoruidStreamer, Margaret, u5718186en_AU
local.contributor.authoruidIreland, Michael, u5544212en_AU
local.contributor.authoruidBento (Da Silva Bento), Joao, u1007677en_AU
local.description.notesImported from ARIESen_AU
local.identifier.absfor020110 - Stellar Astronomy and Planetary Systemsen_AU
local.identifier.absseo970102 - Expanding Knowledge in the Physical Sciencesen_AU
local.identifier.ariespublicationu4485658xPUB1598en_AU
local.identifier.citationvolume480en_AU
local.identifier.doi10.1093/mnras/sty1881en_AU
local.identifier.scopusID2-s2.0-85055157406
local.identifier.thomsonID000442567900092
local.identifier.uidSubmittedByu4485658en_AU
local.publisher.urlhttps://www.wiley.com/en-gben_AU
local.type.statusPublished Versionen_AU

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