Revisiting the Red Giant Branch Hosts KOI-3886 and iota Draconis. Detailed Asteroseismic Modeling and Consolidated Stellar Parameters

• Tipo: Artigo em Revista Científica Internacional
• Data: 2023

Autores

Campante, TL (Autor) FCUP; Li, TD (Autor) Outra; Ong, JMJ (Autor) Outra; Corsaro, E (Autor) Outra; Cunha, MS (Autor) FCUP; Bedding, TR (Autor) Outra; Bossini, D (Autor) Outra; Breton, SN (Autor) Outra; Buzasi, DL (Autor) Outra; Chaplin, WJ (Autor) Outra; Deal, M (Autor) Outra; Garcia, RA (Autor) Outra; Hill, ML (Autor) Outra; Hon, M (Autor) Outra; Huber, D (Autor) Outra; Jiang, C (Autor) Outra; Kane, SR (Autor) Outra; Kayhan, C (Autor) Outra; Kuszlewicz, JS (Autor) Outra; Lillo-Box, J (Autor) Outra; Mathur, S (Autor) Outra; Monteiro, MJPFG (Autor) FCUP; Pereira, F (Autor) Outra; N.C. Santos (Autor) FCUP; Serenelli, A (Autor) Outra; Stello, D (Autor) Outra

Revista

Título: Astronomical Journal

Vol. 165

Página Final: 214

ISSN: 0004-6256

Editora: American Astronomical Society

Indexação

ISI Web of Knowledge - 1 Citação

Scopus

Outras Informações

ID Authenticus: P-00Y-B89

DOI: 10.3847/1538-3881/acc9c1

Abstract (EN): 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 iota Draconis, making use of end-of-mission Kepler (KOI-3886) and multisector TESS (iota 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.

Idioma: Inglês

Tipo (Avaliação Docente): Científica

Nº de páginas: 21