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Title: Dependence of convective boundary mixing on boundary properties and turbulence strength

Abstract

Convective boundary mixing is one of the major uncertainties in stellar evolution. In order to study its dependence on boundary properties and turbulence strength in a controlled way, we computed a series of 3D hydrodynamical simulations of stellar convection during carbon burning with a varying boosting factor of the driving luminosity. Our 3D implicit large eddy simulations were computed with the PROMPI code. Here, we performed a mean field analysis of the simulations within the Reynolds-averaged Navier–Stokes framework. Both the vertical rms velocity within the convective region and the bulk Richardson number of the boundaries are found to scale with the driving luminosity as expected from theory: $$v ∝ L^{1/3}$$ and RiB ∝$$ L^{-2/3}$$, respectively. The positions of the convective boundaries were estimated through the composition profiles across them, and the strength of convective boundary mixing was determined by analysing the boundaries within the framework of the entrainment law. We find that the entrainment is approximately inversely proportional to the bulk Richardson number, RiB (∝$$Ri^{-α}_{B},α ~ 0.75$$). Although the entrainment law does not encompass all the processes occurring at boundaries, our results support the use of the entrainment law to describe convective boundary mixing in 1D models, at least for the advanced phases. Finally, the next steps and challenges ahead are also discussed.

Authors:
ORCiD logo [1];  [2];  [3];  [4];  [5];  [1]
  1. Astrophysics Group, Lennard-Jones Laboratories, Keele University, Keele ST5 5BG, UK
  2. Astrophysics Group, Lennard-Jones Laboratories, Keele University, Keele ST5 5BG, UK, Kavli IPMU (WPI), The University of Tokyo, Kashiwa, Chiba 277-8583, Japan
  3. Department of Astronomy, University of Arizona, Tucson, AZ 85721, USA, Karagozian & Case, Inc., 700 N. Brand Blvd. Suite 700, Glendale, CA, 91203, USA
  4. Department of Astronomy, University of Arizona, Tucson, AZ 85721, USA
  5. Astrophysics Group, Lennard-Jones Laboratories, Keele University, Keele ST5 5BG, UK, Geneva Observatory, University of Geneva, Ch. Maillettes 51, CH-1290 Versoix, Switzerland
Publication Date:
Research Org.:
Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States). National Energy Research Scientific Computing Center (NERSC)
Sponsoring Org.:
USDOE
OSTI Identifier:
1494376
Alternate Identifier(s):
OSTI ID: 1529946
Grant/Contract Number:  
AC02-05CH11231
Resource Type:
Published Article
Journal Name:
Monthly Notices of the Royal Astronomical Society
Additional Journal Information:
Journal Name: Monthly Notices of the Royal Astronomical Society Journal Volume: 484 Journal Issue: 4; Journal ID: ISSN 0035-8711
Publisher:
Oxford University Press
Country of Publication:
United Kingdom
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; convection; hydrodynamics; ISM:evolution

Citation Formats

Cristini, A., Hirschi, R., Meakin, C., Arnett, D., Georgy, C., and Walkington, I. Dependence of convective boundary mixing on boundary properties and turbulence strength. United Kingdom: N. p., 2019. Web. doi:10.1093/mnras/stz312.
Cristini, A., Hirschi, R., Meakin, C., Arnett, D., Georgy, C., & Walkington, I. Dependence of convective boundary mixing on boundary properties and turbulence strength. United Kingdom. doi:10.1093/mnras/stz312.
Cristini, A., Hirschi, R., Meakin, C., Arnett, D., Georgy, C., and Walkington, I. Fri . "Dependence of convective boundary mixing on boundary properties and turbulence strength". United Kingdom. doi:10.1093/mnras/stz312.
@article{osti_1494376,
title = {Dependence of convective boundary mixing on boundary properties and turbulence strength},
author = {Cristini, A. and Hirschi, R. and Meakin, C. and Arnett, D. and Georgy, C. and Walkington, I.},
abstractNote = {Convective boundary mixing is one of the major uncertainties in stellar evolution. In order to study its dependence on boundary properties and turbulence strength in a controlled way, we computed a series of 3D hydrodynamical simulations of stellar convection during carbon burning with a varying boosting factor of the driving luminosity. Our 3D implicit large eddy simulations were computed with the PROMPI code. Here, we performed a mean field analysis of the simulations within the Reynolds-averaged Navier–Stokes framework. Both the vertical rms velocity within the convective region and the bulk Richardson number of the boundaries are found to scale with the driving luminosity as expected from theory: $v ∝ L^{1/3}$ and RiB ∝$ L^{-2/3}$, respectively. The positions of the convective boundaries were estimated through the composition profiles across them, and the strength of convective boundary mixing was determined by analysing the boundaries within the framework of the entrainment law. We find that the entrainment is approximately inversely proportional to the bulk Richardson number, RiB (∝$Ri^{-α}_{B},α ~ 0.75$). Although the entrainment law does not encompass all the processes occurring at boundaries, our results support the use of the entrainment law to describe convective boundary mixing in 1D models, at least for the advanced phases. Finally, the next steps and challenges ahead are also discussed.},
doi = {10.1093/mnras/stz312},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 4,
volume = 484,
place = {United Kingdom},
year = {2019},
month = {2}
}

Journal Article:
Free Publicly Available Full Text
Publisher's Version of Record
DOI: 10.1093/mnras/stz312

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