J/A+A/628/A29 Stellar models grids (Z=0.0134-0.00134) 0.8-35Msun (Claret, 2019)
Updating the theoretical tidal evolution constants:
Apsidal motion and the moment of inertia.
Claret A
<Astron. Astrophys. 628, A29 (2019)>
=2019A&A...628A..29C 2019A&A...628A..29C (SIMBAD/NED BibCode)
ADC_Keywords: Models, evolutionary
Keywords: binaries: eclipsing - binaries: general - stars: evolution -
stars: interiors - planetary systems
Abstract:
The theoretical apsidal motion constants are key tools to investigate
the stellar interiors in close eccentric binary systems. In addition,
these constants and the moment of inertia are also important to
investigate the tidal evolution of close binary stars as well as of
exo-planetary systems. The aim of the paper is to present new
evolutionary models, based on the MESA package, that include the
internal structure constants (k2, k3, and k4), the radius of
gyration, and the gravitational potential energy for configurations
computed from the pre-main-sequence (PMS) up to the first ascent giant
branch or beyond. The calculations are available for the three
metallicities [Fe/H] = 0.00, -0.50, and -1.00, which take the recent
investigations in less metallic environments into account. This new
set of models replaces the old ones, published about 15 years ago,
using the code GRANADA. Core overshooting was taken into account using
the mass-fov relationship, which was derived semi-empirically for
models more massive than 1.2M☉. The differential equations
governing the apsidal motion constants, moment of inertia, and the
gravitational potential energy were integrated simultaneously through
a fifth-order Runge-Kutta method with a tolerance level of 10-7.
The resulting models (from 0.8 up to 35.0M☉) are presented
in 54 tables for the three metallicities, containing the usual
characteristics of an evolutionary model (age, initial masses,
logTeff, logg, and logL), the constants of internal structure
(k2, k3, and k4), the radius of gyration β and the
factor α that is related with the gravitational potential
energy.
Description:
The stellar models were computed using the Modules for Experiments in
Stellar Astrophysics package (MESA; Paxton et al. 2011, 2013, 2015)
version 7385, which does not include the effects of rotation. The
adopted mixing-length parameter alphaMLT was 1.84 (the
solar-calibrated value).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
grid.dat 56 54 Summary of parameters
tables/* . 55 Original tables (2-55) explanations (README)
z0013.dat 127 119662 * Z=0.0013 models (log(M)=0.80-35.0)
z0042.dat 127 103234 * Z=0.0042 models (log(M)=0.80-35.0)
z0134.dat 127 172250 * Z=0.0134 models (log(M)=0.80-35.0)
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Note on z0013.dat, z0042.dat, z0134.dat: For all models, alphaMLT=1.84.
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See also:
J/A+A/424/919 : New grids of stellar models I (Claret, 2004)
J/A+A/440/647 : New grids of stellar models II (Claret, 2005)
Byte-by-byte Description of file: grid.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- --- [Mi=]
4- 8 F5.2 Msun Mi [0.80/35.0] Initial mass
10- 11 A2 --- --- [Z=]
12- 17 F6.4 --- Z [0.0013/0.0134] Z initial composition
19- 22 A4 --- --- [fov= ]
23- 27 F5.3 --- fov ? Overshooting free parameter, fov
29- 48 A20 --- n_fov "without overshooting"
50- 56 A7 --- FileName Original filename with result
(in subdirectory tables)
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Byte-by-byte Description of file: z0013.dat z0042.dat z0134.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 F5.2 --- Mi [0.80/35.0] Initial mass
7- 12 F6.4 --- Z [0.0013/0.0134] Z initial composition
14- 18 F5.3 --- fov [0/0.016] Overshooting free parameter, fov
(0 for no overshooting)
22- 35 E14.8 yr Age Age of the models
38- 45 F8.5 Msun Mass Actual mass of the model
48- 55 F8.5 [Lsun] log(L) Log (Total luminosity)
58- 65 F8.5 [K] log(Teff) Log (Effective temperature)
68- 75 F8.5 [cm/s2] log(g) Log (Surface gravity)
78- 85 F8.5 --- logk2 Log(Apsidal motion constant (j=2))
88- 95 F8.5 --- logk3 Log(Apsidal motion constant (j=3))
98-105 F8.5 --- logk4 Log(Apsidal motion constant (j=4))
106-117 E12.5 --- apot apot = -EpxR/GM2
120-127 F8.5 --- beta Fractional gyration radius
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Acknowledgements:
Antonio Claret claret(at)iaa.es
(End) Patricia Vannier [CDS] 24-Jul-2019