J/ApJ/764/21 Stellar evolutionary models with 13-120Msun (Chieffi+, 2013)
Pre-supernova evolution of rotating solar metallicity stars in the mass range
13-120M☉ and their explosive yields.
Chieffi A., Limongi M.
<Astrophys. J., 764, 21 (2013)>
=2013ApJ...764...21C 2013ApJ...764...21C
ADC_Keywords: Models, evolutionary ; Supernovae ; Stars, masses
Keywords: stars: evolution; stars: interiors; stars: massive; stars: rotation;
supernovae: general
Abstract:
We present the first set of a new generation of models of massive
stars with a solar composition extending between 13 and 120M☉,
computed with and without the effects of rotation. We included two
instabilities induced by rotation: the meridional circulation and the
shear instability. We implemented two alternative schemes to treat the
transport of the angular momentum: the advection-diffusion formalism
and the simpler purely diffusive one. The full evolution from the
pre-main sequence up to the pre-supernova stage is followed in detail
with a very extended nuclear network. The explosive yields are
provided for a variety of possible mass cuts and are available at the
Web site http://www.iasf-roma.inaf.it/orfeo/public_html. We find that
both the He and the CO core masses are larger than those of their
non-rotating counterparts. Also the C abundance left by the He burning
is lower than in the non-rotating case, especially for stars with an
initial mass of 13-25M☉, and this affects the final mass-radius
relation, basically the final binding energy, at the pre-supernova
stage. The elemental yields produced by a generation of stars rotating
initially at 300km/s do not change substantially with respect to those
produced by a generation of non-rotating massive stars, the main
differences being a slight overproduction of the weak s-component and
a larger production of F. Since rotation also affects the mass-loss
rate, either directly or indirectly, we find substantial differences
in the lifetimes as O-type and Wolf-Rayet subtypes between the
rotating and non-rotating models. The maximum mass exploding as
Type IIP supernova ranges between 15 and 20M ☉ in both sets of
models (this value depends basically on the larger mass-loss rates in
the red supergiant phase due to the inclusion of the dust-driven
wind). This limiting value is in remarkably good agreement with
current estimates.
Description:
The mechanical and thermal distortions induced by rotation have been
included in our stellar evolutionary code (FRANEC) following the
scheme proposed by Kippenhahn & Thomas (1970stro.coll...20K) and
Pinsonneault et al. (1989ApJ...338..424P 1989ApJ...338..424P) that can be considered as a
general approach (Heger et al. 2000ApJ...528..368H 2000ApJ...528..368H; Meynet & Maeder
1997A&A...321..465M 1997A&A...321..465M). We also included two rotation-driven
instabilities, namely, the meridional circulation and the shear,
following the schemes proposed either by Meynet & Maeder
(2003A&A...404..975M 2003A&A...404..975M, and references therein) or by Heger et al.
(2000ApJ...528..368H 2000ApJ...528..368H, and references therein).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 125 63 *Main evolutionary properties of the rotating models
table2.dat 92 63 Main evolutionary properties of the non-rotating
models
table7.dat 87 294 Explosion properties and ejected masses of the
rotating models
table8.dat 87 294 Explosion properties and ejected masses of the
non rotating models
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Note on table1.dat: initial equatorial velocity of vini=300km/s.
See section 4 for further explanations.
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See also:
J/A+A/558/A131 : Model spectra of hot stars at the pre-SN stage (Groh+, 2013)
J/A+A/558/A103 : Stellar models with rotation, Z=0.002 (Georgy+, 2013)
J/A+A/553/A24 : Models for rotating stars (Georgy+, 2013)
J/ApJS/199/38 : Presupernova evolution (Limongi+, 2012)
J/A+A/537/A146 : Stellar models with rotation, Z=0.014 (Ekstrom+, 2012)
J/A+A/530/A115 : Rotating massive MS stars evolutionary models (Brott+, 2011)
J/A+A/496/841 : VLT-FLAMES survey of massive stars (Hunter+, 2009)
J/A+A/479/541 : VLT-FLAMES survey of massive stars (Hunter+, 2008)
J/A+A/471/625 : VLT-FLAMES survey of massive stars (Trundle+, 2007)
J/A+A/466/277 : VLT-FLAMES survey of massive stars (Hunter+, 2007)
Byte-by-byte Description of file: table[12].dat
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Bytes Format Units Label Explanations
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1- 3 I3 Msun Mini [13/120] Initial mass
5- 7 A3 --- Phase Evolutionary phase (H, He, C, Ne, O, Si, PSN)
9- 15 E7.3 yr Time Lifetime on Phase
17- 21 F5.2 Msun MCC [0/93]? Mass size of the convective core
23- 26 F4.2 [K] Teff [3.5/5.4] log of average effective temperature
28- 31 F4.2 [Lsun] logL [4.5/6.3] log of average luminosity
33- 37 F5.2 Msun Mass [7.3/53] Total mass
39- 43 F5.2 Msun MHe [0/46] He core mass
45- 49 F5.2 Msun MCO [0/25] CO core mass
51- 57 E7.3 --- Hsup [0/0.8] Surface abundance of H in mass
fraction Hsup
59- 65 E7.3 --- Hesup [0.2/1] Surface abundance of He in mass
fraction Hesup
67- 74 E8.3 --- Nsup Surface abundance of N in mass fraction Nsup
76- 83 E8.3 --- N/C N/C surface ratio
85- 92 E8.3 --- N/O N/O surface ratio
94-100 E7.3 km/s Veq [0.03/228]? Equatorial velocity
(only for table 1)
102-109 E8.3 s-1 Oms ? Surface angular velocity ωsup
(only for table 1)
111-117 E7.3 --- O/Ocr [0.001/0.7]? Ratio of the surface angular
velocity to the critical angular velocity
ω/ωc (only for table 1)
119-125 E7.3 10+53g.cm2/s Jtot [0.01/0.7]? Total angular momentum Jtot
(only for table 1)
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Byte-by-byte Description of file: table[78].dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- Model Model parameter at 2.5e+4s after explosion (1)
8- 15 E8.2 Msun M13 Model value for Mini=13M☉
17- 24 E8.2 Msun M15 Model value for Mini=15M☉
26- 33 E8.2 Msun M20 Model value for Mini=20M☉
35- 42 E8.2 Msun M25 Model value for Mini=25M☉
44- 51 E8.2 Msun M30 Model value for Mini=30M☉
53- 60 E8.2 Msun M40 Model value for Mini=40M☉
62- 69 E8.2 Msun M60 Model value for Mini=60M☉
71- 78 E8.2 Msun M80 Model value for Mini=80M☉
80- 87 E8.2 Msun M120 Model value for Mini=120M☉
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Note (1): Explanations on some parameters:
Ekin = kinetic energy of the ejecta resulting from the full ejection
of the mass above the Fe core (in 1051erg=1044J)
Mcut = mass coordinate which separates the ejecta from the compact remnant
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 23-Oct-2014