J/A+A/622/A50 Calibrated grid of rotating single star models (Higgins+, 2019)
Massive star evolution: rotation, winds, and overshooting vectors in the
mass-luminosity plane. I. A calibrated grid of rotating single star models.
Higgins E.R., Vink J.S.
<Astron. Astrophys. 622, A50 (2019)>
=2019A&A...622A..50H 2019A&A...622A..50H (SIMBAD/NED BibCode)
ADC_Keywords: Models, evolutionary ; Mass loss
Keywords: stars: massive - evolution - mass loss
Abstract:
Massive star evolution is dominated by various physical effects,
including mass loss, overshooting, and rotation, but the prescriptions
of their effects are poorly constrained, even affecting our
understanding of the main sequence.
We aim to constrain massive star evolution models using the unique
testbed eclipsing binary HD166734 with new grids of MESA stellar
evolution models, adopting calibrated prescriptions of overshooting,
mass loss, and rotation.
We introduce a novel tool: the "mass-luminosity plane" or "M-L plane",
as an equivalent to the traditional HR diagram, utilising it to
reproduce the testbed binary HD166734 with newly calibrated MESA
stellar evolution models for single stars.
We can only reproduce the Galactic binary system with an enhanced
amount of core overshooting (alphaov=0.5), mass loss, and rotational
mixing. We can utilise the gradient in the M-L plane to constrain the
amount of mass loss to 0.5-1.5 times the standard Vink et al.
(2001A&A...369..574V 2001A&A...369..574V) prescriptions, and we can exclude extreme
reduction or multiplication factors. The extent of the vectors in the
M-L plane leads us to conclude that the amount of core overshooting is
larger than is normally adopted in contemporary massive star evolution
models. We furthermore conclude that rotational mixing is mandatory to
get the nitrogen abundance ratios between the primary and secondary
components to be correct (3:1) in our testbed binary system.
Our calibrated grid of models, alongside our new M-L plane approach,
present the possibility of a widened main sequence due to an increased
demand for core overshooting. The increased amount of core
overshooting is not only needed to explain the extended main sequence,
but the enhanced overshooting is also needed to explain the location
of the upper-luminosity limit of the red supergiants. Finally, the
increased amount of core overshooting has - via the compactness
parameter - implications for supernova explodibility.
Description:
We provide the history.data file for each model with renamed files of
the format
'Initial-massInitial-rotation-rateovershooting-alpha.data' for
initial masses 8-60M, initial rotation rates 0-500km/s, and
overshooting alpha of 0.1 or 0.5. Each file is set up via the mesa
defaults 'history_columns.list' format with column headers
assigned. Each model includes the version number of mesa - 8845,
initial mass, initial metallicity (z), and limits for reported
burning. Key stellar parameters such as age, mass, effective
temperature, luminosity, radius, log g, compactness parameter, core
masses, rotational parameters, and surface abundances are included
among many others. Full details can be found via column headers on
line 6. Full documentation for 'Modules for Experiments in Stellar
Astrophysics' MESA can be found via the instrumentation papers:
Paxton et al. (2011ApJS..192....3P 2011ApJS..192....3P, 2013ApJS..208....4P 2013ApJS..208....4P,
2015ApJS..220...15P 2015ApJS..220...15P and 2018ApJS..234...34P 2018ApJS..234...34P).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 25 144 List of models
history_columns.list 115 740 Explanation of the labels
models/* . 144 Models
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See also:
http://193.63.77.2:8383/armaghobservatoryplanetarium/published/erin_higgins.php : Models Home Page
Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 2 I2 Msun Mini [8/60] Initial mass
4- 6 I3 km/s omega [0/500] Initial rotation rate
8- 10 F3.1 --- al.ov [0.1/0.5] Overshooting, alpha
12- 25 A14 --- FileName Name of the file in subdirectory models
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Acknowledgements:
Erin Higgins, Erin.Higgins(at)Armagh.ac.uk
J.S. Vink, jsv(at)arm.ac.uk
(End) Patricia Vannier [CDS] 13-Dec-2018