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http://hdl.handle.net/10261/339739
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dc.contributor.author | Campante, Tiago L. | es_ES |
dc.contributor.author | Li, Tanda | es_ES |
dc.contributor.author | Ong, Jia Mian Joel | es_ES |
dc.contributor.author | Corsaro, Enrico | es_ES |
dc.contributor.author | Cunha, Margarida S. | es_ES |
dc.contributor.author | Bedding, Timothy R. | es_ES |
dc.contributor.author | Bossini, Diego | es_ES |
dc.contributor.author | Breton, Sylvain N. | es_ES |
dc.contributor.author | Buzasi, Derek | es_ES |
dc.contributor.author | Chaplin, William J. | es_ES |
dc.contributor.author | Deal, Morgan | es_ES |
dc.contributor.author | García, Rafael A. | es_ES |
dc.contributor.author | Hill, Michelle L. | es_ES |
dc.contributor.author | Hon, Marc | es_ES |
dc.contributor.author | Huber, Daniel | es_ES |
dc.contributor.author | Jiang, Chen | es_ES |
dc.contributor.author | Kane, Stephen R. | es_ES |
dc.contributor.author | Kayhan, Cenk | es_ES |
dc.contributor.author | Kuszlewicz, James S. | es_ES |
dc.contributor.author | Lillo-Box, Jorge | es_ES |
dc.contributor.author | Mathur, Savita | es_ES |
dc.contributor.author | Monteiro, Mario J.P.F.G. | es_ES |
dc.contributor.author | Pereira, Filipe | es_ES |
dc.contributor.author | Santos, Nuno C. | es_ES |
dc.contributor.author | Serenelli, Aldo | es_ES |
dc.contributor.author | Stello, Dennis | es_ES |
dc.date.accessioned | 2023-11-27T12:44:13Z | - |
dc.date.available | 2023-11-27T12:44:13Z | - |
dc.date.issued | 2023 | - |
dc.identifier.citation | Astronomical Journal 165(5): 214 (2023) | es_ES |
dc.identifier.issn | 0004-6256 | - |
dc.identifier.uri | http://hdl.handle.net/10261/339739 | - |
dc.description.abstract | Asteroseismology is playing an increasingly important role in the characterization of red giant host stars and their planetary systems. Here, we conduct detailed asteroseismic modeling of the evolved red giant branch (RGB) hosts KOI-3886 and ι Draconis, making use of end-of-mission Kepler (KOI-3886) and multisector TESS (ι Draconis) time-series photometry. We also model the benchmark star KIC 8410637, a member of an eclipsing binary, thus providing a direct test to the seismic determination. We test the impact of adopting different sets of observed modes as seismic constraints. Inclusion of ℓ = 1 and 2 modes improves the precision of the stellar parameters, albeit marginally, compared to adopting radial modes alone, with 1.9%–3.0% (radius), 5%–9% (mass), and 19%–25% (age) reached when using all p-dominated modes as constraints. Given the very small spacing of adjacent dipole mixed modes in evolved RGB stars, the sparse set of observed g-dominated modes is not able to provide extra constraints, further leading to highly multimodal posteriors. Access to multiyear time-series photometry does not improve matters, with detailed modeling of evolved RGB stars based on (lower-resolution) TESS data sets attaining a precision commensurate with that based on end-of-mission Kepler data. Furthermore, we test the impact of varying the atmospheric boundary condition in our stellar models. We find the mass and radius estimates to be insensitive to the description of the near-surface layers, at the expense of substantially changing both the near-surface structure of the best-fitting models and the values of associated parameters like the initial helium abundance, Yi. Attempts to measure Yi from seismic modeling of red giants may thus be systematically dependent on the choice of atmospheric physics. | es_ES |
dc.description.sponsorship | This work was supported by Fundação para a Ciência e a Tecnologia (FCT) through research grants UIDB/04434/2020 and UIDP/04434/2020. This work was supported by FCT through national funds (PTDC/FIS-AST/30389/2017) and by FEDER through COMPETE2020 (POCI-01-0145-FEDER-030389). T.L.C. is supported by FCT in the form of a work contract (CEECIND/00476/2018). T.L. is supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (CartographY; Grant Agreement no. 804752). J.M.J.O. acknowledges partial support by NASA grant 80NSSC19K0374, awarded to Sarbani Basu, and from NASA through the NASA Hubble Fellowship grant HST-HF2-51517.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. M.S.C. is supported by FCT in the form of a work contract (CEECIND/ 02619/2017). T.R.B. was supported by the Australian Research Council (DP210103119). S.N.B. and R.A.G. acknowledge support from the PLATO CNES grant. M.D. is supported by national funds through FCT in the form of a work contract. D.H. acknowledges support from the Alfred P. Sloan Foundation and the National Aeronautics and Space Administration (80NSSC19K0597, 80NSSC21K0652). C.J. is supported by a grant from the Max Planck Society to prepare for the scientific exploitation of the PLATO mission. C.K. acknowledges support from Erciyes University Scientific Research Projects Coordination Unit through grant DOSAP MAP-2020-9749. J.L.-B. acknowledges financial support received from the “la Caixa” Foundation under Marie Skłodowska-Curie fellowship with code LCF/BQ/PI20/11760023 and the Spanish State Research Agency (AEI) projects PID2019-107061GB-C61 and MDM-2017-0737. S.M. acknowledges support from the Spanish Ministry of Science and Innovation (MICINN) with the Ramón y Cajal fellowship no. RYC-2015-17697 and grant no. PID2019-107187GB-I00, and through AEI under the Severo Ochoa Centres of Excellence Programme 2020–2023 (CEX2019-000920-S). A.S. is supported by grants PID2019-108709GB-I00 of the Spanish MICINN and María de Maeztu CEX2020-001058-M. | es_ES |
dc.format | application/pdf | es_ES |
dc.language.iso | eng | es_ES |
dc.publisher | IOP Publishing | es_ES |
dc.relation | info:eu-repo/grantAgreement/EC/H2020/804752 | es_ES |
dc.relation | info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2019-107061GB-C61/ES/CONTRIBUCION DEL CAB+INTA%2FSGE A LA MISION ESPACIAL PLATO2.0. FASE C%2FD-1/ | es_ES |
dc.relation | info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2019-107187GB-I00/ES/SEISMOLOGY AND STELLAR ROTATION WITH TESS/ | es_ES |
dc.relation | info:eu-repo/grantAgreement/AEI//CEX2019-000920-S | es_ES |
dc.relation | info:eu-repo/grantAgreement/AEI//CEX2020-001058-M | es_ES |
dc.relation | info:eu-repo/grantAgreement/MINECO//RYC-2015-17697/ES/RYC-2015-17697/ | es_ES |
dc.relation.isversionof | Publisher's version | es_ES |
dc.rights | openAccess | es_ES |
dc.title | Revisiting the red giant branch hosts KOI-3886 and ι draconis. Detailed asteroseismic modeling and consolidated stellar parameters | es_ES |
dc.type | artículo | es_ES |
dc.identifier.doi | 10.3847/1538-3881/acc9c1 | - |
dc.description.peerreviewed | Peer reviewed | es_ES |
dc.relation.publisherversion | https://doi.org/10.3847/1538-3881/acc9c1 | es_ES |
dc.rights.license | http://creativecommons.org/licenses/by/4.0/ | es_ES |
dc.contributor.funder | Fundação para a Ciência e a Tecnologia (Portugal) | es_ES |
dc.contributor.funder | European Commission | es_ES |
dc.contributor.funder | European Research Council | es_ES |
dc.contributor.funder | National Aeronautics and Space Administration (US) | es_ES |
dc.contributor.funder | Australian Research Council | es_ES |
dc.contributor.funder | Fundación la Caixa | es_ES |
dc.contributor.funder | Alfred P. Sloan Foundation | es_ES |
dc.contributor.funder | Agencia Estatal de Investigación (España) | es_ES |
dc.contributor.funder | Ministerio de Ciencia, Innovación y Universidades (España) | es_ES |
dc.contributor.funder | Ministerio de Economía y Competitividad (España) | es_ES |
dc.relation.csic | Sí | es_ES |
oprm.item.hasRevision | no ko 0 false | * |
dc.identifier.funder | http://dx.doi.org/10.13039/100000879 | es_ES |
dc.identifier.funder | http://dx.doi.org/10.13039/501100000923 | es_ES |
dc.identifier.funder | http://dx.doi.org/10.13039/501100000780 | es_ES |
dc.identifier.funder | http://dx.doi.org/10.13039/501100000781 | es_ES |
dc.identifier.funder | http://dx.doi.org/10.13039/501100001871 | es_ES |
dc.identifier.funder | http://dx.doi.org/10.13039/501100003329 | es_ES |
dc.identifier.funder | http://dx.doi.org/10.13039/100000104 | es_ES |
dc.identifier.funder | http://dx.doi.org/10.13039/501100011033 | es_ES |
dc.type.coar | http://purl.org/coar/resource_type/c_6501 | es_ES |
item.grantfulltext | open | - |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.fulltext | With Fulltext | - |
item.cerifentitytype | Publications | - |
item.languageiso639-1 | en | - |
item.openairetype | artículo | - |
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