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  Testing Stellar Evolution with Asteroseismic Inversions of a Main-sequence Star Harboring a Small Convective Core

Bellinger, E. P., Basu, S., Hekker, S., & Christensen-Dalsgaard, J. (2019). Testing Stellar Evolution with Asteroseismic Inversions of a Main-sequence Star Harboring a Small Convective Core. The Astrophysical Journal, 885(2): 143. doi:10.3847/1538-4357/ab4a0d.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0005-587F-B Version Permalink: http://hdl.handle.net/21.11116/0000-0005-5880-7
Genre: Journal Article

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 Creators:
Bellinger, Earl P., Author
Basu, Sarbani, Author
Hekker, Saskia1, Author              
Christensen-Dalsgaard, Jørgen, Author
Affiliations:
1Max Planck Research Group in Stellar Ages and Galactic Evolution (SAGE), Max Planck Institute for Solar System Research, Max Planck Society, ou_2265636              

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Free keywords: Asteroseismology ; Stellar astronomy ; Stellar oscillations ; Stellar evolution ; Stellar physics ; Stellar evolutionary models ; Solar analogs ; Stellar interiors ; Stellar cores ; Stellar structures ; Stellar convective zones ; Astrophysical processes
 Abstract: The goal of stellar evolution theory is to predict the structure of stars throughout their lifetimes. Usually, these predictions can be assessed only indirectly, for example by comparing predicted and observed effective temperatures and luminosities. Thanks now to asteroseismology, which can reveal the internal structure of stars, it becomes possible to compare the predictions from stellar evolution theory to actual stellar structures. In this work, we present an inverse analysis of the oscillation data from the solar-type star KIC 6225718, which was observed by the Kepler space observatory during its nominal mission. As its mass is about 20% greater than solar, this star is predicted to transport energy by convection in its nuclear-burning core. We find significant differences between the predicted and actual structure of the star in the radiative interior near to the convective core. In particular, the predicted sound speed is higher than observed in the deep interior of the star, and too low at a fractional radius of 0.25 and beyond. The cause of these discrepancies is unknown, and is not remedied by known physics in the form of convective overshooting or elemental diffusion.

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Language(s): eng - English
 Dates: 2019
 Publication Status: Published online
 Pages: -
 Publishing info: -
 Table of Contents: -
 Rev. Method: Peer
 Identifiers: DOI: 10.3847/1538-4357/ab4a0d
 Degree: -

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Title: The Astrophysical Journal
Source Genre: Journal
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Publ. Info: Bristol; Vienna : IOP Publishing; IAEA
Pages: - Volume / Issue: 885 (2) Sequence Number: 143 Start / End Page: - Identifier: ISSN: 0004-637X
CoNE: https://pure.mpg.de/cone/journals/resource/954922828215_3