K Dwarf Radius Inflation and a 10 Gyr Spin-down Clock Unveiled through Asteroseismology of HD 219134 from the Keck Planet Finder
We present the first asteroseismic analysis of the K3 V planet host HD 219134 based on four consecutive nights of radial velocities collected with the Keck Planet Finder. We apply Gold deconvolution to the power spectrum to disentangle modes from side lobes in the spectral window and extract 25 mode...
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| author | Yaguang Li Daniel Huber J. M. Joel Ong Jennifer van Saders R. R. Costa Jens Reersted Larsen Sarbani Basu Timothy R. Bedding Fei Dai Ashley Chontos Theron W. Carmichael Daniel Hey Hans Kjeldsen Marc Hon Tiago L. Campante Mário J. P. F. G. Monteiro Mia Sloth Lundkvist Nicholas Saunders Howard Isaacson Andrew W. Howard Steven R. Gibson Samuel Halverson Kodi Rider Arpita Roy Ashley D. Baker Jerry Edelstein Chris Smith Benjamin J. Fulton Josh Walawender |
| author_facet | Yaguang Li Daniel Huber J. M. Joel Ong Jennifer van Saders R. R. Costa Jens Reersted Larsen Sarbani Basu Timothy R. Bedding Fei Dai Ashley Chontos Theron W. Carmichael Daniel Hey Hans Kjeldsen Marc Hon Tiago L. Campante Mário J. P. F. G. Monteiro Mia Sloth Lundkvist Nicholas Saunders Howard Isaacson Andrew W. Howard Steven R. Gibson Samuel Halverson Kodi Rider Arpita Roy Ashley D. Baker Jerry Edelstein Chris Smith Benjamin J. Fulton Josh Walawender |
| author_sort | Yaguang Li |
| collection | DOAJ |
| description | We present the first asteroseismic analysis of the K3 V planet host HD 219134 based on four consecutive nights of radial velocities collected with the Keck Planet Finder. We apply Gold deconvolution to the power spectrum to disentangle modes from side lobes in the spectral window and extract 25 mode frequencies with spherical degrees 0 ≤ ℓ ≤ 3. We derive the fundamental properties using five different evolutionary-modeling pipelines and report a mass of 0.763 ± 0.020 (stat) ± 0.007 (sys) M _⊙ , a radius of 0.748 ± 0.007 (stat) ± 0.002 (sys) R _⊙ , and an age of 10.151 ± 1.520 (stat) ± 0.810 (sys) Gyr. Compared to the interferometric radius 0.783 ± 0.005 R _⊙ , the asteroseismic radius is 4% smaller at the 4 σ level—a discrepancy not easily explained by known interferometric systematics, modeling assumptions on atmospheric boundary conditions and mixing lengths, magnetic fields, or tidal heating. HD 219134 is the first main-sequence star cooler than 5000 K with an asteroseismic age estimate and will serve as a critical calibration point for stellar spin-down relations. We show that existing calibrated prescriptions for angular momentum loss, incorporating weakened magnetic braking with asteroseismically constrained stellar parameters, accurately reproduce the observed rotation period. Additionally, we revised the masses and radii of the super-Earths in the system, which support their having Earth-like compositions. Finally, we confirm that the oscillation amplitude in radial velocity scales as ( L / M ) ^1.5 in K dwarfs, in contrast to the ( L / M ) ^0.7 relation observed in G dwarfs. These findings provide significant insights into the structure and angular momentum loss of K-type stars. |
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| spelling | doaj-art-7fda2342b6b44a5f9f4d6aee7a88ba322025-08-20T02:33:09ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-01984212510.3847/1538-4357/adc737K Dwarf Radius Inflation and a 10 Gyr Spin-down Clock Unveiled through Asteroseismology of HD 219134 from the Keck Planet FinderYaguang Li0https://orcid.org/0000-0003-3020-4437Daniel Huber1https://orcid.org/0000-0001-8832-4488J. M. Joel Ong2https://orcid.org/0000-0001-7664-648XJennifer van Saders3https://orcid.org/0000-0002-4284-8638R. R. Costa4https://orcid.org/0009-0008-6039-6381Jens Reersted Larsen5https://orcid.org/0009-0006-0423-2353Sarbani Basu6https://orcid.org/0000-0002-6163-3472Timothy R. Bedding7https://orcid.org/0000-0001-5222-4661Fei Dai8https://orcid.org/0000-0002-8958-0683Ashley Chontos9https://orcid.org/0000-0003-1125-2564Theron W. Carmichael10https://orcid.org/0000-0001-6416-1274Daniel Hey11https://orcid.org/0000-0003-3244-5357Hans Kjeldsen12https://orcid.org/0000-0002-9037-0018Marc Hon13https://orcid.org/0000-0003-2400-6960Tiago L. Campante14https://orcid.org/0000-0002-4588-5389Mário J. P. F. G. Monteiro15https://orcid.org/0000-0003-0513-8116Mia Sloth Lundkvist16https://orcid.org/0000-0002-8661-2571Nicholas Saunders17https://orcid.org/0000-0003-2657-3889Howard Isaacson18https://orcid.org/0000-0002-0531-1073Andrew W. Howard19https://orcid.org/0000-0001-8638-0320Steven R. Gibson20https://orcid.org/0009-0004-4454-6053Samuel Halverson21https://orcid.org/0000-0003-1312-9391Kodi Rider22Arpita Roy23https://orcid.org/0000-0001-8127-5775Ashley D. Baker24https://orcid.org/0000-0002-6525-7013Jerry Edelstein25https://orcid.org/0009-0002-2419-8819Chris Smith26Benjamin J. Fulton27https://orcid.org/0000-0003-3504-5316Josh Walawender28https://orcid.org/0000-0002-6092-8295Institute for Astronomy, University of Hawai’i , 2680 Woodlawn Drive, Honolulu, HI 96822, USA ; yaguangl@hawaii.eduInstitute for Astronomy, University of Hawai’i , 2680 Woodlawn Drive, Honolulu, HI 96822, USA ; yaguangl@hawaii.eduInstitute for Astronomy, University of Hawai’i , 2680 Woodlawn Drive, Honolulu, HI 96822, USA ; yaguangl@hawaii.eduInstitute for Astronomy, University of Hawai’i , 2680 Woodlawn Drive, Honolulu, HI 96822, USA ; yaguangl@hawaii.eduInstituto de Astrofísica e Ciências do Espaço, Universidade do Porto , Rua das Estrelas, 4150-762 Porto, Portugal; 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, 8000 Aarhus C, DenmarkDepartment of Astronomy, Yale University , New Haven, CT 06511, USASydney Institute for Astronomy (SIfA), School of Physics, University of Sydney , NSW 2006, AustraliaInstitute for Astronomy, University of Hawai’i , 2680 Woodlawn Drive, Honolulu, HI 96822, USA ; yaguangl@hawaii.eduDepartment of Astrophysical Sciences, Princeton University , 4 Ivy Lane, Princeton, NJ 08540, USAInstitute for Astronomy, University of Hawai’i , 2680 Woodlawn Drive, Honolulu, HI 96822, USA ; yaguangl@hawaii.eduInstitute for Astronomy, University of Hawai’i , 2680 Woodlawn Drive, Honolulu, HI 96822, USA ; yaguangl@hawaii.eduStellar Astrophysics Centre (SAC), Department of Physics and Astronomy , Aarhus University, Ny Munkegade 120, 8000 Aarhus C, DenmarkKavli Institute for Astrophysics and Space Research , Massachusetts Institute of Technology, Cambridge, MA 02139, USAInstituto de Astrofísica e Ciências do Espaço, Universidade do Porto , Rua das Estrelas, 4150-762 Porto, Portugal; 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; 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, 8000 Aarhus C, DenmarkInstitute for Astronomy, University of Hawai’i , 2680 Woodlawn Drive, Honolulu, HI 96822, USA ; yaguangl@hawaii.eduDepartment of Astronomy, 501 Campbell Hall, University of California , Berkeley, CA 94720, USADepartment of Astronomy, California Institute of Technology , Pasadena, CA 91125, USACaltech Optical Observatories, California Institute of Technology , Pasadena, CA 91125, USAJet Propulsion Laboratory, California Institute of Technology , 4800 Oak Grove Drive, Pasadena, CA 91109, USASpace Sciences Laboratory, University of California , Berkeley, CA 94720, USAAstrophysics & Space Institute , Schmidt Sciences, New York, NY 10011, USACaltech Optical Observatories, California Institute of Technology , Pasadena, CA 91125, USASpace Sciences Laboratory, University of California , Berkeley, CA 94720, USASpace Sciences Laboratory, University of California , Berkeley, CA 94720, USANASA Exoplanet Science Institute/Caltech-IPAC, California Institute of Technology , Pasadena, CA 91125, USAW. M. Keck Observatory , 65-1120 Mamalahoa Highway, Kamuela, HI 96743, USAWe present the first asteroseismic analysis of the K3 V planet host HD 219134 based on four consecutive nights of radial velocities collected with the Keck Planet Finder. We apply Gold deconvolution to the power spectrum to disentangle modes from side lobes in the spectral window and extract 25 mode frequencies with spherical degrees 0 ≤ ℓ ≤ 3. We derive the fundamental properties using five different evolutionary-modeling pipelines and report a mass of 0.763 ± 0.020 (stat) ± 0.007 (sys) M _⊙ , a radius of 0.748 ± 0.007 (stat) ± 0.002 (sys) R _⊙ , and an age of 10.151 ± 1.520 (stat) ± 0.810 (sys) Gyr. Compared to the interferometric radius 0.783 ± 0.005 R _⊙ , the asteroseismic radius is 4% smaller at the 4 σ level—a discrepancy not easily explained by known interferometric systematics, modeling assumptions on atmospheric boundary conditions and mixing lengths, magnetic fields, or tidal heating. HD 219134 is the first main-sequence star cooler than 5000 K with an asteroseismic age estimate and will serve as a critical calibration point for stellar spin-down relations. We show that existing calibrated prescriptions for angular momentum loss, incorporating weakened magnetic braking with asteroseismically constrained stellar parameters, accurately reproduce the observed rotation period. Additionally, we revised the masses and radii of the super-Earths in the system, which support their having Earth-like compositions. Finally, we confirm that the oscillation amplitude in radial velocity scales as ( L / M ) ^1.5 in K dwarfs, in contrast to the ( L / M ) ^0.7 relation observed in G dwarfs. These findings provide significant insights into the structure and angular momentum loss of K-type stars.https://doi.org/10.3847/1538-4357/adc737Stellar rotationK dwarf starsStellar oscillations |
| spellingShingle | Yaguang Li Daniel Huber J. M. Joel Ong Jennifer van Saders R. R. Costa Jens Reersted Larsen Sarbani Basu Timothy R. Bedding Fei Dai Ashley Chontos Theron W. Carmichael Daniel Hey Hans Kjeldsen Marc Hon Tiago L. Campante Mário J. P. F. G. Monteiro Mia Sloth Lundkvist Nicholas Saunders Howard Isaacson Andrew W. Howard Steven R. Gibson Samuel Halverson Kodi Rider Arpita Roy Ashley D. Baker Jerry Edelstein Chris Smith Benjamin J. Fulton Josh Walawender K Dwarf Radius Inflation and a 10 Gyr Spin-down Clock Unveiled through Asteroseismology of HD 219134 from the Keck Planet Finder The Astrophysical Journal Stellar rotation K dwarf stars Stellar oscillations |
| title | K Dwarf Radius Inflation and a 10 Gyr Spin-down Clock Unveiled through Asteroseismology of HD 219134 from the Keck Planet Finder |
| title_full | K Dwarf Radius Inflation and a 10 Gyr Spin-down Clock Unveiled through Asteroseismology of HD 219134 from the Keck Planet Finder |
| title_fullStr | K Dwarf Radius Inflation and a 10 Gyr Spin-down Clock Unveiled through Asteroseismology of HD 219134 from the Keck Planet Finder |
| title_full_unstemmed | K Dwarf Radius Inflation and a 10 Gyr Spin-down Clock Unveiled through Asteroseismology of HD 219134 from the Keck Planet Finder |
| title_short | K Dwarf Radius Inflation and a 10 Gyr Spin-down Clock Unveiled through Asteroseismology of HD 219134 from the Keck Planet Finder |
| title_sort | k dwarf radius inflation and a 10 gyr spin down clock unveiled through asteroseismology of hd 219134 from the keck planet finder |
| topic | Stellar rotation K dwarf stars Stellar oscillations |
| url | https://doi.org/10.3847/1538-4357/adc737 |
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