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_{sun}_ and their explosive yields. Chieffi A., Limongi M. =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_{sun}_, 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_{sun}_, 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 _{sun}_ 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) that can be considered as a general approach (Heger et al. 2000ApJ...528..368H; Meynet & Maeder 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, and references therein) or by Heger et al. (2000ApJ...528..368H, and references therein). File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- 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 -------------------------------------------------------------------------------- Note on table1.dat: initial equatorial velocity of v_ini_=300km/s. See section 4 for further explanations. -------------------------------------------------------------------------------- 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 -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 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 H_sup_ 59- 65 E7.3 --- Hesup [0.2/1] Surface abundance of He in mass fraction He_sup_ 67- 74 E8.3 --- Nsup Surface abundance of N in mass fraction N_sup_ 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 {omega}_sup_ (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 {omega}/{omega}_c_ (only for table 1) 119-125 E7.3 10+53g.cm2/s Jtot [0.01/0.7]? Total angular momentum J_tot_ (only for table 1) -------------------------------------------------------------------------------- Byte-by-byte Description of file: table[78].dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 6 A6 --- Model Model parameter at 2.5e+4s after explosion (1) 8- 15 E8.2 Msun M13 Model value for Mini=13M_{sun}_ 17- 24 E8.2 Msun M15 Model value for Mini=15M_{sun}_ 26- 33 E8.2 Msun M20 Model value for Mini=20M_{sun}_ 35- 42 E8.2 Msun M25 Model value for Mini=25M_{sun}_ 44- 51 E8.2 Msun M30 Model value for Mini=30M_{sun}_ 53- 60 E8.2 Msun M40 Model value for Mini=40M_{sun}_ 62- 69 E8.2 Msun M60 Model value for Mini=60M_{sun}_ 71- 78 E8.2 Msun M80 Model value for Mini=80M_{sun}_ 80- 87 E8.2 Msun M120 Model value for Mini=120M_{sun}_ -------------------------------------------------------------------------------- Note (1): Explanations on some parameters: E_kin_ = kinetic energy of the ejecta resulting from the full ejection of the mass above the Fe core (in 10^51^erg=10^44^J) M_cut_ = mass coordinate which separates the ejecta from the compact remnant -------------------------------------------------------------------------------- History: From electronic version of the journal ================================================================================ (End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 23-Oct-2014