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  Convective boundary mixing in low- and intermediate-mass stars – I. Core properties from pressure-mode asteroseismology

Angelou, G. C., Bellinger, E. P., Hekker, S., Mints, A., Elsworth, Y., Basu, S., et al. (2020). Convective boundary mixing in low- and intermediate-mass stars – I. Core properties from pressure-mode asteroseismology. Monthly Notices of the Royal Astronomical Society, 493(4), 4987-5004. doi:10.1093/mnras/staa390.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0006-F50A-B Version Permalink: http://hdl.handle.net/21.11116/0000-0006-F50B-A
Genre: Journal Article

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 Creators:
Angelou, George C.1, Author              
Bellinger, Earl P, Author
Hekker, Saskia1, Author              
Mints, Alexey1, Author              
Elsworth, Yvonne, Author
Basu, Sarbani, Author
Weiss, Achim, 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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 Abstract: Convective boundary mixing (CBM) is ubiquitous in stellar evolution. It is a necessary ingredient in the models in order to match observational constraints from clusters, binaries, and single stars alike. We compute ‘effective overshoot’ measures that reflect the extent of mixing and which can differ significantly from the input overshoot values set in the stellar evolution codes. We use constraints from pressure modes to infer the CBM properties of Kepler and CoRoT main-sequence and subgiant oscillators, as well as in two radial velocity targets (Procyon A and α Cen A). Collectively, these targets allow us to identify how measurement precision, stellar spectral type, and overshoot implementation impact the asteroseismic solution. With these new measures, we find that the ‘effective overshoot’ for most stars is in line with physical expectations and calibrations from binaries and clusters. However, two F-stars in the CoRoT field (HD 49933 and HD 181906) still necessitate high overshoot in the models. Due to short mode lifetimes, mode identification can be difficult in these stars. We demonstrate that an incongruence between the radial and non-radial modes drives the asteroseismic solution to extreme structures with highly efficient CBM as an inevitable outcome. Understanding the cause of seemingly anomalous physics for such stars is vital for inferring accurate stellar parameters from TESS data with comparable timeseries length.

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Language(s): eng - English
 Dates: 2020
 Publication Status: Published in print
 Pages: -
 Publishing info: -
 Table of Contents: -
 Rev. Type: Peer
 Identifiers: DOI: 10.1093/mnras/staa390
 Degree: -

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Title: Monthly Notices of the Royal Astronomical Society
  Other : Mon. Not. R. Astron. Soc.
Source Genre: Journal
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Publ. Info: Oxford : Oxford University Press
Pages: - Volume / Issue: 493 (4) Sequence Number: - Start / End Page: 4987 - 5004 Identifier: ISSN: 1365-8711
CoNE: https://pure.mpg.de/cone/journals/resource/1000000000024150