Probing the shape of the mixing profile and of the thermal structure at the convective core boundary through asteroseismology
| Autor: | Kyle Augustson, M. G. Pedersen, Mathias Michielsen, Stéphane Mathis, Conny Aerts |
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| Přispěvatelé: | Instituut voor Sterrenkunde [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud university [Nijmegen], Support from the CNES PLATO grant at CEA/DAp, European Project: 670519,H2020,ERC-2014-ADG,MAMSIE(2016), European Project: 647383,H2020,ERC-2014-CoG,SPIRE(2015), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Radboud University [Nijmegen] |
| Jazyk: | angličtina |
| Rok vydání: | 2019 |
| Předmět: |
oscillations [stars]
Astronomy MODE-IDENTIFICATION Astrophysics stars: interiors 01 natural sciences photometric [techniques] techniques: photometric massive [stars] Stars: oscillations (including pulsations) Astrophysics::Solar and Stellar Astrophysics Stellar structure 010303 astronomy & astrophysics Mixing (physics) convection Physics Oscillation Astrophysics::Instrumentation and Methods for Astrophysics OVERSHOOT stars: massive Temperature gradient Astrophysics - Solar and Stellar Astrophysics A-TYPE STARS Physical Sciences Astrophysics::Earth and Planetary Astrophysics stars: oscillations Convection FOS: Physical sciences asteroseismology Astronomy & Astrophysics Asteroseismology Computer Science::Digital Libraries 0103 physical sciences PHOTOMETRY MASSES Solar and Stellar Astrophysics (astro-ph.SR) interiors [stars] Science & Technology 010308 nuclear & particles physics Astronomy and Astrophysics Light curve Astrophysics - Astrophysics of Galaxies Physics::History of Physics SIMULATIONS Stars Space and Planetary Science STELLAR EVOLUTION Astrophysics of Galaxies (astro-ph.GA) ROTATION BRITE [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] |
| Zdroj: | Astronomy and Astrophysics-A&A Astronomy and Astrophysics-A&A, EDP Sciences, 2019, 628, pp.A76. ⟨10.1051/0004-6361/201935754⟩ Astronomy & Astrophysics Astronomy and Astrophysics-A&A, 2019, 628, pp.A76. ⟨10.1051/0004-6361/201935754⟩ Astronomy & Astrophysics, 628, pp. 1-11 Astronomy & Astrophysics, 628, 1-11 |
| ISSN: | 0004-6361 1432-0746 |
| DOI: | 10.1051/0004-6361/201935754⟩ |
| Popis: | Aims: We investigate from a theoretical perspective if space asteroseismology can be used to distinguish between different thermal structures and shapes of the near-core mixing profiles for different types of coherent oscillation modes in massive stars with convective cores, and if this capacity depends on the evolutionary stage of the models along the main sequence. Methods: We compute 1D stellar structure and evolution models for four different prescriptions of the mixing and temperature gradient in the near-core region. Their effect on the frequencies of dipole prograde gravity modes in both Slowly Pulsating B and β Cep stars is investigated, as well as for pressure modes in β Cep stars. Results: A comparison between the mode frequencies of the different models at various stages during the main sequence evolution reveals that they are more sensitive to a change in temperature gradient than to the exact shape of the mixing profile in the near-core region. Depending on the duration of the observed light curve, one can distinguish between either just the temperature gradient, or also between the shapes of the mixing coefficient. The relative frequency differences are in general larger for more evolved models, and are largest for the higher-frequency pressure modes in β Cep stars. Conclusions:In order to unravel the core boundary mixing and thermal structure of the near-core region, one must have asteroseismic masses and radii with ∼1% relative precision for hundreds of stars. The given publication date is the date of acceptance |
| Databáze: | OpenAIRE |
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