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Title: Evolving R Coronae Borealis stars with mesa

Abstract

ABSTRACT The R Coronae Borealis (RCB) stars are rare hydrogen-deficient, carbon-rich supergiants. They undergo extreme, irregular declines in brightness of many magnitudes due to the formation of thick clouds of carbon dust. It is thought that RCB stars result from the mergers of CO/He white dwarf (WD) binaries. We constructed post-merger spherically symmetric models computed with the mesa code, and then followed the evolution into the region of the Hertzsprung-Russell (H−R) diagram where the RCB stars are located. We also investigated nucleosynthesis in the dynamically accreting material of CO/He WD mergers which may provide a suitable environment for significant production of 18O and the very low 16O/18O values observed. We have also discovered that the N abundance depends sensitively on the peak temperature in the He-burning shell. Our mesa modelling consists of engineering the star by adding He-WD material to an initial CO-WD model, and then following the post-merger evolution using a nuclear-reaction network to match the observed RCB abundances as it expands and cools to become an RCB star. These new models are more physical because they include rotation, mixing, mass-loss, and nucleosynthesis within mesa. We follow the later evolution beyond the RCB phase to determine the stars’ likelymore » lifetimes. The relative numbers of known RCB and extreme helium stars correspond well to the lifetimes predicted from the mesa models. In addition, most of computed abundances agree very well with the observed range of abundances for the RCB class.« less

Authors:
 [1];  [2]; ORCiD logo [2];  [2];  [2]
  1. Department of Physics and Astronomy, Louisiana State University, Baton Rouge, LA 70803, USA, Triangle Universities Nuclear Lab, Duke University, Durham, NC 27710, USA
  2. Department of Physics and Astronomy, Louisiana State University, Baton Rouge, LA 70803, USA
Publication Date:
Sponsoring Org.:
USDOE
OSTI Identifier:
1532815
Grant/Contract Number:  
DE–SC0014231
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: 488 Journal Issue: 1; Journal ID: ISSN 0035-8711
Publisher:
Oxford University Press
Country of Publication:
United Kingdom
Language:
English

Citation Formats

Lauer, Amber, Chatzopoulos, Emmanouil, Clayton, Geoffrey C., Frank, Juhan, and Marcello, Dominic C. Evolving R Coronae Borealis stars with mesa. United Kingdom: N. p., 2019. Web. doi:10.1093/mnras/stz1732.
Lauer, Amber, Chatzopoulos, Emmanouil, Clayton, Geoffrey C., Frank, Juhan, & Marcello, Dominic C. Evolving R Coronae Borealis stars with mesa. United Kingdom. doi:10.1093/mnras/stz1732.
Lauer, Amber, Chatzopoulos, Emmanouil, Clayton, Geoffrey C., Frank, Juhan, and Marcello, Dominic C. Thu . "Evolving R Coronae Borealis stars with mesa". United Kingdom. doi:10.1093/mnras/stz1732.
@article{osti_1532815,
title = {Evolving R Coronae Borealis stars with mesa},
author = {Lauer, Amber and Chatzopoulos, Emmanouil and Clayton, Geoffrey C. and Frank, Juhan and Marcello, Dominic C.},
abstractNote = {ABSTRACT The R Coronae Borealis (RCB) stars are rare hydrogen-deficient, carbon-rich supergiants. They undergo extreme, irregular declines in brightness of many magnitudes due to the formation of thick clouds of carbon dust. It is thought that RCB stars result from the mergers of CO/He white dwarf (WD) binaries. We constructed post-merger spherically symmetric models computed with the mesa code, and then followed the evolution into the region of the Hertzsprung-Russell (H−R) diagram where the RCB stars are located. We also investigated nucleosynthesis in the dynamically accreting material of CO/He WD mergers which may provide a suitable environment for significant production of 18O and the very low 16O/18O values observed. We have also discovered that the N abundance depends sensitively on the peak temperature in the He-burning shell. Our mesa modelling consists of engineering the star by adding He-WD material to an initial CO-WD model, and then following the post-merger evolution using a nuclear-reaction network to match the observed RCB abundances as it expands and cools to become an RCB star. These new models are more physical because they include rotation, mixing, mass-loss, and nucleosynthesis within mesa. We follow the later evolution beyond the RCB phase to determine the stars’ likely lifetimes. The relative numbers of known RCB and extreme helium stars correspond well to the lifetimes predicted from the mesa models. In addition, most of computed abundances agree very well with the observed range of abundances for the RCB class.},
doi = {10.1093/mnras/stz1732},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 1,
volume = 488,
place = {United Kingdom},
year = {2019},
month = {6}
}

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This content will become publicly available on June 27, 2020
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