J/A+A/553/A24 Models for rotating stars (Georgy+, 2013)
Populations of rotating stars.
I. Models from 1.7 to 15M☉ at Z = 0.014, 0.006, and 0.002 with
Ω/Ωcrit between 0 and 1.
Georgy C., Ekstrom S., Granada A., Meynet G., Mowlavi N., Eggenberger P.,
Maeder A.
<Astron. Astrophys. 553, A24 (2013)>
=2013A&A...553A..24G 2013A&A...553A..24G
ADC_Keywords: Models, evolutionary ; Stars, Be ; Mass loss
Keywords: stars: general - stars: evolution - stars: rotation -
stars: emission-line, Be - stars: mass-loss
Abstract:
B-type stars are known to rotate at various velocities, including very
fast rotators near the critical velocity as the Be stars.
In this paper, we provide stellar models covering the mass range
between 1.7 to 15M☉, which includes the typical mass of known Be
stars, at Z=0.014, 0.006 and 0.002 and for an extended range of
initial velocities on the zero-age main sequence. We use the Geneva
stellar-evolution code including the effects of shellular rotation and
with a numerical treatment that has been improved in order for the
code to track in a precise way the variation of the angular momentum
content of the star as it changes under the influence of radiative
winds and/or mechanical mass loss. We discuss the impact of the
initial rotation rate on the tracks in the Hertzsprung-Russell
diagram, the main-sequence (MS) lifetimes, the evolution of the
surface rotation and abundances, as well as on the ejected masses of
various isotopes. Among the new results obtained from the present grid
we have that: 1) fast rotating stars with initial masses around
1.7M☉ present at the beginning of the core hydrogen-burning
phase quite small convective cores with respect to their slowly
rotating counterparts. This fact may be interesting to keep in mind in
the frame of the asteroseismic studies of such stars; 2) the contrast
between the core and surface angular velocity is higher in slower
rotating stars. The values presently obtained are quite in the range
of the very few values obtained for B-type stars from
asteroseismology; 3) at Z=0.002, the stars in the mass range of 1.7 to
3M☉ with a mean velocity on the MS of the order of 150km/s show
N/H enhancement superior to 0.2dex at mid-MS, and superior to 0.4dex
at the end of the MS phase. At solar metallicity the corresponding
values are below 0.2dex at any time in the MS. An extended database of
stellar models containing 270 evolutionary tracks is provided to the
community.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
models.dat 570 108000 Evolutionary tracks for 270 combinations of
initial M, Z and Ω/Ωcrit
files.tar 1386 108379 All the individual files for the 270
evolutionary tracks
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See also:
J/A+A/291/155 : Rotating neutron stars models .I. (Salgado+, 1994)
J/A+AS/108/455 : Rotating neutron stars models. II. (Salgado+, 1994)
J/A+A/346/586 : Rotating models of A and F stars (Perez Hernandez+, 1999)
J/A+A/530/A115 : Rotating massive MS stars evolutionary models (Brott+, 2011)
J/A+A/537/A146 : Stellar models with rotation. 0.8<M<120, Z=0.014
(Ekstrom+, 2012)
Byte-by-byte Description of file: models.dat
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Bytes Format Units Label Explanations
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1- 4 F4.1 Msun Mini Initial mass (1)
6- 10 F5.3 --- Zini Initial Z abundance (1)
12- 15 F4.2 --- OOcini Ω/Ωcrit value (1)
17- 19 I3 --- Line Number of selected point
21- 42 E22.15 yr Time Age
44- 54 F11.6 Msun Mass Actual mass in solar masses
55- 64 F10.6 [Lsun] logL log(luminosity) in solar units
66- 74 F9.6 [K] logTe log(effective temperature)
76- 89 E14.7 --- X H surface abundance (mass fraction)
91-104 E14.7 --- Y He surface abundance (mass fraction)
106-119 E14.7 --- C12 12C surface abundance (mass fraction)
121-134 E14.7 --- C13 13C surface abundance (mass fraction)
136-149 E14.7 --- N14 14N surface abundance (mass fraction)
151-164 E14.7 --- O16 16O surface abundance (mass fraction)
166-179 E14.7 --- O17 17O surface abundance (mass fraction)
181-194 E14.7 --- O18 18O surface abundance (mass fraction)
196-209 E14.7 --- Ne20 20Ne surface abundance (mass fraction)
211-224 E14.7 --- Ne22 22Ne surface abundance (mass fraction)
226-235 E10.3 --- Al26 26Al surface abundance (mass fraction)
237-243 F7.4 --- QCC convective core mass fraction
245-253 F9.6 [K] logTu log(uncorrected Teff) (WR stars only)
255-262 F8.3 [Msun/yr] logdM/dt log(mass loss rate)
264-272 F9.6 [g/cm3] log(rhoc) log(central density)
274-282 F9.6 [K] logTc log(central temperature)
284-297 E14.7 --- Xc H central abundance (mass fraction)
299-312 E14.7 --- Yc 4He central abundance (mass fraction)
314-327 E14.7 --- C12c 12C central abundance (mass fraction)
329-342 E14.7 --- C13c 13C central abundance (mass fraction)
344-357 E14.7 --- N14c 14N central abundance (mass fraction)
359-372 E14.7 --- O16c 16O central abundance (mass fraction)
374-387 E14.7 --- O17c 17O central abundance (mass fraction)
389-402 E14.7 --- O18c 18O central abundance (mass fraction)
404-417 E14.7 --- Ne20c 20Ne central abundance (mass fraction)
419-432 E14.7 --- Ne22c 22Ne central abundance (mass fraction)
434-443 E10.3 --- Al26c 26Al central abundance (mass fraction)
445-454 E10.3 s-1 Omegas Surface angular velocity
456-465 E10.3 s-1 Omegac Central angular velocity
467-476 E10.3 --- RpRe Oblateness (polar/equatorial radius)
478-487 E10.3 --- dM/dtR Rotational dM/dt correction factor
489-497 E9.2 km/s vcrit1 First critical velocity (Ω-limit)
499-507 E9.2 km/s vcrit2 Second critical velocity
(ΩΓ-limit)
509-517 E9.2 km/s veq Equatorial velocity
519-527 F9.6 --- OOc Ωsurf/Ωcrit
529-537 F9.6 --- Gedd Eddington factor ΓEdd
539-552 E14.7 Msun/yr dM/dtm Mechanical equatorial dM/dt
554-570 E17.10 10+53g.cm2/s Ltot Total angular momentum
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Note (1): Initial values:
* Initial mass values:
1.7 2.0 2.5 3.0 4.0 5.0 7.0 9.0 12.0 15.0
* Initial Z values:
0.002 0.006 0.014
* Initial Ω/Ωcrit values:
0.00 0.10 0.30 0.50 0.60 0.70 0.80 0.90 0.95
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Acknowledgements:
Cyril Georgy, c.georgy (at)keele.ac.uk
(End) Cyril Georgy [Keele University], Patricia Vannier [CDS] 08-Mar-2013