Revisiting the Red Giant Branch Hosts KOI-3886 and ι Draconis. Detailed Asteroseismic Modeling and Consolidated Stellar Parameters
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)...
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astronomical Journal |
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| Online Access: | https://doi.org/10.3847/1538-3881/acc9c1 |
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| author | Tiago L. Campante Tanda Li J. M. Joel Ong Enrico Corsaro Margarida S. Cunha Timothy R. Bedding Diego Bossini Sylvain N. Breton Derek L. Buzasi William J. Chaplin Morgan Deal Rafael A. García Michelle L. Hill Marc Hon Daniel Huber Chen Jiang Stephen R. Kane Cenk Kayhan James S. Kuszlewicz Jorge Lillo-Box Savita Mathur Mário J. P. F. G. Monteiro Filipe Pereira Nuno C. Santos Aldo Serenelli Dennis Stello |
| author_facet | Tiago L. Campante Tanda Li J. M. Joel Ong Enrico Corsaro Margarida S. Cunha Timothy R. Bedding Diego Bossini Sylvain N. Breton Derek L. Buzasi William J. Chaplin Morgan Deal Rafael A. García Michelle L. Hill Marc Hon Daniel Huber Chen Jiang Stephen R. Kane Cenk Kayhan James S. Kuszlewicz Jorge Lillo-Box Savita Mathur Mário J. P. F. G. Monteiro Filipe Pereira Nuno C. Santos Aldo Serenelli Dennis Stello |
| author_sort | Tiago L. Campante |
| collection | DOAJ |
| description | 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, Y _i . Attempts to measure Y _i from seismic modeling of red giants may thus be systematically dependent on the choice of atmospheric physics. |
| first_indexed | 2024-03-12T03:22:25Z |
| format | Article |
| id | doaj.art-933892b91fcd4fa298bf766335340f8f |
| institution | Directory Open Access Journal |
| issn | 1538-3881 |
| language | English |
| last_indexed | 2024-03-12T03:22:25Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astronomical Journal |
| spelling | doaj.art-933892b91fcd4fa298bf766335340f8f2023-09-03T13:52:19ZengIOP PublishingThe Astronomical Journal1538-38812023-01-01165521410.3847/1538-3881/acc9c1Revisiting the Red Giant Branch Hosts KOI-3886 and ι Draconis. Detailed Asteroseismic Modeling and Consolidated Stellar ParametersTiago L. Campante0https://orcid.org/0000-0002-4588-5389Tanda Li1https://orcid.org/0000-0001-6396-2563J. M. Joel Ong2https://orcid.org/0000-0001-7664-648XEnrico Corsaro3https://orcid.org/0000-0001-8835-2075Margarida S. Cunha4https://orcid.org/0000-0001-8237-7343Timothy R. Bedding5https://orcid.org/0000-0001-5222-4661Diego Bossini6https://orcid.org/0000-0002-9480-8400Sylvain N. Breton7https://orcid.org/0000-0003-0377-0740Derek L. Buzasi8https://orcid.org/0000-0002-1988-143XWilliam J. Chaplin9https://orcid.org/0000-0002-5714-8618Morgan Deal10https://orcid.org/0000-0001-6774-3587Rafael A. García11https://orcid.org/0000-0002-8854-3776Michelle L. Hill12https://orcid.org/0000-0002-0139-4756Marc Hon13https://orcid.org/0000-0003-2400-6960Daniel Huber14https://orcid.org/0000-0001-8832-4488Chen Jiang15https://orcid.org/0000-0002-7614-1665Stephen R. Kane16https://orcid.org/0000-0002-7084-0529Cenk Kayhan17https://orcid.org/0000-0001-9198-2289James S. Kuszlewicz18https://orcid.org/0000-0002-3322-5279Jorge Lillo-Box19https://orcid.org/0000-0003-3742-1987Savita Mathur20https://orcid.org/0000-0002-0129-0316Mário J. P. F. G. Monteiro21https://orcid.org/0000-0003-0513-8116Filipe Pereira22https://orcid.org/0000-0002-2157-7146Nuno C. Santos23https://orcid.org/0000-0003-4422-2919Aldo Serenelli24https://orcid.org/0000-0001-6359-2769Dennis Stello25https://orcid.org/0000-0002-4879-3519Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto , Rua das Estrelas, 4150-762 Porto, Portugal ; tiago.campante@astro.up.pt; Departamento de Física e Astronomia, Faculdade de Ciências da Universidade do Porto , Rua do Campo Alegre, s/n, 4169-007 Porto, PortugalDepartment of Astronomy, Beijing Normal University , Beijing, 100875, People’s Republic of China ; litanda@bnu.edu.cn; School of Physics and Astronomy, University of Birmingham , Edgbaston, Birmingham B15 2TT, UK; Stellar Astrophysics Centre (SAC), Department of Physics and Astronomy, Aarhus University , Ny Munkegade 120, DK-8000 Aarhus C, DenmarkInstitute for Astronomy, University of Hawai’i , 2680 Woodlawn Dr., Honolulu, HI 96822, USA ; joelong@hawaii.edu; Department of Astronomy, Yale University , 52 Hillhouse Ave., New Haven, CT 06511, USAINAF—Osservatorio Astrofisico di Catania , via S. Sofia 78, I-95123 Catania, ItalyInstituto de Astrofísica e Ciências do Espaço, Universidade do Porto , Rua das Estrelas, 4150-762 Porto, Portugal ; tiago.campante@astro.up.pt; Departamento de Física e Astronomia, Faculdade de Ciências da Universidade do Porto , Rua do Campo Alegre, s/n, 4169-007 Porto, PortugalStellar Astrophysics Centre (SAC), Department of Physics and Astronomy, Aarhus University , Ny Munkegade 120, DK-8000 Aarhus C, Denmark; Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney , NSW 2006, AustraliaInstituto de Astrofísica e Ciências do Espaço, Universidade do Porto , Rua das Estrelas, 4150-762 Porto, Portugal ; tiago.campante@astro.up.ptINAF—Osservatorio Astrofisico di Catania , via S. Sofia 78, I-95123 Catania, Italy; AIM, CEA, CNRS, Université Paris-Saclay , Université Paris Diderot, Sorbonne Paris Cité, F-91191 Gif-sur-Yvette, FranceDepartment of Chemistry and Physics, Florida Gulf Coast University , 10501 FGCU Blvd.S., Fort Myers, FL 33965, USASchool of Physics and Astronomy, University of Birmingham , Edgbaston, Birmingham B15 2TT, UK; Stellar Astrophysics Centre (SAC), Department of Physics and Astronomy, Aarhus University , Ny Munkegade 120, DK-8000 Aarhus C, DenmarkInstituto de Astrofísica e Ciências do Espaço, Universidade do Porto , Rua das Estrelas, 4150-762 Porto, Portugal ; tiago.campante@astro.up.ptAIM, CEA, CNRS, Université Paris-Saclay , Université Paris Diderot, Sorbonne Paris Cité, F-91191 Gif-sur-Yvette, FranceDepartment of Earth and Planetary Sciences, University of California Riverside , 900 University Ave., Riverside, CA 92521, USAInstitute for Astronomy, University of Hawai’i , 2680 Woodlawn Dr., Honolulu, HI 96822, USA ; joelong@hawaii.edu; School of Physics, The University of New South Wales , Sydney NSW 2052, AustraliaInstitute for Astronomy, University of Hawai’i , 2680 Woodlawn Dr., Honolulu, HI 96822, USA ; joelong@hawaii.eduMax-Planck-Institut für Sonnensystemforschung , Justus-von-Liebig-Weg 3, D-37077 Göttingen, GermanyDepartment of Earth and Planetary Sciences, University of California Riverside , 900 University Ave., Riverside, CA 92521, USADepartment of Astronomy and Space Sciences, Erciyes University , 38030, Kayseri, TurkeyCenter for Astronomy (Landessternwarte), Heidelberg University , Königstuhl 12, D-69118 Heidelberg, GermanyCentro de Astrobiología (CAB, CSIC-INTA) , Depto. de Astrofísica, ESAC Campus E-28692 Villanueva de la Cañada (Madrid), SpainInstituto de Astrofísica de Canarias (IAC) , E-38205 La Laguna, Tenerife, Spain; Universidad de La Laguna (ULL) , Departamento de Astrofísica, E-38206 La Laguna, Tenerife, SpainInstituto de Astrofísica e Ciências do Espaço, Universidade do Porto , Rua das Estrelas, 4150-762 Porto, Portugal ; tiago.campante@astro.up.pt; Departamento de Física e Astronomia, Faculdade de Ciências da Universidade do Porto , Rua do Campo Alegre, s/n, 4169-007 Porto, PortugalInstituto de Astrofísica e Ciências do Espaço, Universidade do Porto , Rua das Estrelas, 4150-762 Porto, Portugal ; tiago.campante@astro.up.pt; Departamento de Física e Astronomia, Faculdade de Ciências da Universidade do Porto , Rua do Campo Alegre, s/n, 4169-007 Porto, PortugalInstituto de Astrofísica e Ciências do Espaço, Universidade do Porto , Rua das Estrelas, 4150-762 Porto, Portugal ; tiago.campante@astro.up.pt; Departamento de Física e Astronomia, Faculdade de Ciências da Universidade do Porto , Rua do Campo Alegre, s/n, 4169-007 Porto, PortugalInstitute of Space Sciences (ICE, CSIC) Campus UAB , Carrer de Can Magrans, s/n, E-08193, Bellaterra, Spain; Institut d’Estudis Espacials de Catalunya (IEEC) , Carrer del Gran Capità, 2-4, E-08034, Barcelona, SpainStellar Astrophysics Centre (SAC), Department of Physics and Astronomy, Aarhus University , Ny Munkegade 120, DK-8000 Aarhus C, Denmark; School of Physics, The University of New South Wales , Sydney NSW 2052, AustraliaAsteroseismology 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, Y _i . Attempts to measure Y _i from seismic modeling of red giants may thus be systematically dependent on the choice of atmospheric physics.https://doi.org/10.3847/1538-3881/acc9c1AsteroseismologyStellar evolutionFundamental parameters of stars |
| spellingShingle | Tiago L. Campante Tanda Li J. M. Joel Ong Enrico Corsaro Margarida S. Cunha Timothy R. Bedding Diego Bossini Sylvain N. Breton Derek L. Buzasi William J. Chaplin Morgan Deal Rafael A. García Michelle L. Hill Marc Hon Daniel Huber Chen Jiang Stephen R. Kane Cenk Kayhan James S. Kuszlewicz Jorge Lillo-Box Savita Mathur Mário J. P. F. G. Monteiro Filipe Pereira Nuno C. Santos Aldo Serenelli Dennis Stello Revisiting the Red Giant Branch Hosts KOI-3886 and ι Draconis. Detailed Asteroseismic Modeling and Consolidated Stellar Parameters The Astronomical Journal Asteroseismology Stellar evolution Fundamental parameters of stars |
| title | Revisiting the Red Giant Branch Hosts KOI-3886 and ι Draconis. Detailed Asteroseismic Modeling and Consolidated Stellar Parameters |
| title_full | Revisiting the Red Giant Branch Hosts KOI-3886 and ι Draconis. Detailed Asteroseismic Modeling and Consolidated Stellar Parameters |
| title_fullStr | Revisiting the Red Giant Branch Hosts KOI-3886 and ι Draconis. Detailed Asteroseismic Modeling and Consolidated Stellar Parameters |
| title_full_unstemmed | Revisiting the Red Giant Branch Hosts KOI-3886 and ι Draconis. Detailed Asteroseismic Modeling and Consolidated Stellar Parameters |
| title_short | Revisiting the Red Giant Branch Hosts KOI-3886 and ι Draconis. Detailed Asteroseismic Modeling and Consolidated Stellar Parameters |
| title_sort | revisiting the red giant branch hosts koi 3886 and ι draconis detailed asteroseismic modeling and consolidated stellar parameters |
| topic | Asteroseismology Stellar evolution Fundamental parameters of stars |
| url | https://doi.org/10.3847/1538-3881/acc9c1 |
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