Asteroseismology of Massive Stars with the TESS Mission: The Runaway ? Cep Pulsator PHL 346=HN Aqr

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dc.authoridPascual Granado, Javier/0000-0003-0139-6951
dc.authoridPedersen, May Gade/0000-0002-7950-0061
dc.authoridHandler, Gerald/0000-0001-7756-1568
dc.authoridPigulski, Andrzej/0000-0003-2488-6726
dc.authoridDaszynska-Daszkiewicz, Jadwiga/0000-0001-9704-6408
dc.authoridKallinger, Thomas/0000-0003-3627-2561
dc.authoridNiemczura, Ewa/0000-0001-7290-5800
dc.contributor.authorHandler, Gerald
dc.contributor.authorPigulski, Andrzej
dc.contributor.authorDaszynska-Daszkiewicz, Jadwiga
dc.contributor.authorIrrgang, Andreas
dc.contributor.authorKilkenny, David
dc.contributor.authorGuo, Zhao
dc.contributor.authorPrzybilla, Norbert
dc.date.accessioned2025-01-27T21:04:08Z
dc.date.available2025-01-27T21:04:08Z
dc.date.issued2019
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractWe report an analysis of the first known beta Cep pulsator observed by the Transiting Exoplanet Survey Satellite (TESS) mission, the runaway star PHL 346 = HN Aqr. The star, previously known as a singly periodic pulsator, has at least 34 oscillation modes excited, 12 of those in the g-mode domain and 22 p modes. Analysis of archival data implies that the amplitude and frequency of the dominant mode and the stellar radial velocity were variable over time. A binary nature would be inconsistent with the inferred ejection velocity from the Galactic disk of 420 km s(-1), which is too large to be survivable by a runaway binary system. A kinematic analysis of the star results in an age constraint (23 +/- 1 Myr) that can be imposed on asteroseismic modeling and that can be used to remove degeneracies in the modeling process. Our attempts to match the excitation of the observed frequency spectrum resulted in pulsation models that were too young. Hence, asteroseismic studies of runaway pulsators can become vital not only in tracing the evolutionary history of such objects, but to understand the interior structure of massive stars in general. TESS is now opening up these stars for detailed asteroseismic investigation.
dc.description.sponsorshipNASA Explorer Program; Danish National Research Foundation [DNRF106]; ESA PRODEX [PEA 4000119301]; Stellar Astrophysics Centre (SAC) at Aarhus University; TASC/TASOC; ESO programme [383.D-0909(A)]; Polish NCN [2015/18/A/ST9/00578, 2016/21/B/ST9/01126, 2015/17/B/ST9/02082, 2014/13/B/ST9/00902]; STFC [ST/R000603/1]; European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme [670519: MAMSIE]; Spanish MCIU [AYA2015-68012-C2-1-P, SEV2015-0548]; Gobierno de Canarias [2017010115]; STFC [ST/R000603/1, ST/L003910/2] Funding Source: UKRI
dc.description.sponsorshipThis Letter 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. We thank the TESS team and staff and TASC/TASOC for their support of the present work. This work is also based on observations collected at the European Southern Observatory under ESO programme 383.D-0909(A). Funding through the Polish NCN grants 2015/18/A/ST9/00578, 2016/21/B/ST9/01126, 2015/17/B/ST9/02082 and 2014/13/B/ST9/00902 is gratefully acknowledged. G.M.M. acknowledges funding by the STFC consolidated grant ST/R000603/1. The research leading to these results has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement No. 670519: MAMSIE). S.S.-D. acknowledges funding by the Spanish MCIU (projects AYA2015-68012-C2-1-P and SEV2015-0548) and the Gobierno de Canarias (project ProID2017010115). G.H. thanks Daniel Heynderickx for supplying the photometry by Waelkens & Rufener (1988), David Jones for help in retrieving archival data and Andrzej Baran for helpful comments on the manuscript.
dc.identifier.doi10.3847/2041-8213/ab095f
dc.identifier.issn2041-8205
dc.identifier.issn2041-8213
dc.identifier.issue1
dc.identifier.scopus2-s2.0-85063519639
dc.identifier.scopusqualityQ1
dc.identifier.urihttps://doi.org/10.3847/2041-8213/ab095f
dc.identifier.urihttps://hdl.handle.net/20.500.12428/27559
dc.identifier.volume873
dc.identifier.wosWOS:000460065200001
dc.identifier.wosqualityQ1
dc.indekslendigikaynakWeb of Science
dc.indekslendigikaynakScopus
dc.language.isoen
dc.publisherIop Publishing Ltd
dc.relation.ispartofAstrophysical Journal Letters
dc.relation.publicationcategoryinfo:eu-repo/semantics/openAccess
dc.rightsinfo:eu-repo/semantics/openAccess
dc.snmzKA_WoS_20250125
dc.subjectstars: early-type
dc.subjectstars: individual (HN Aqr)
dc.subjectstars: interiors
dc.subjectstars: kinematics and dynamics
dc.subjectstars: massive
dc.subjectstars: oscillations (including pulsations)
dc.titleAsteroseismology of Massive Stars with the TESS Mission: The Runaway ? Cep Pulsator PHL 346=HN Aqr
dc.typeArticle

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