J/ApJ/769/99 Nucleosynthetic yields for stars >12M{sun} (Brown+, 2013) ================================================================================ Nucleosynthetic constraints on the mass of the heaviest supernovae. Brown J.M., Woosley S.E. =2013ApJ...769...99B ================================================================================ ADC_Keywords: Models ; Supernovae ; Abundances Keywords: galaxies: abundances; hydrodynamics; supernovae: general; nuclear reactions, nucleosynthesis, abundances; stars: abundances Abstract: We explore the sensitivity of nucleosynthesis in massive stars to the truncation of supernova explosions above a certain mass. It is assumed that stars of all masses contribute to nucleosynthesis by their pre-explosive winds, but above a certain limiting main sequence mass, M_BH_, the presupernova star becomes a black hole and ejects nothing more. The solar abundances from oxygen to atomic mass 90 are fit quite well assuming no cutoff at all, i.e., by assuming all stars up to 120M_{sun}_ make successful supernovae. Little degradation in the fit occurs if M_BH_ is reduced to 25M_{sun}_. If this limit is reduced further however, the nucleosynthesis of the s-process declines precipitously and the production of species made in the winds, e.g., carbon, becomes unacceptably large compared with elements made in the explosion, e.g., silicon and oxygen. By varying uncertain physics, especially the mass loss rate for massive stars and the rate for the ^22^Ne({alpha},n)^25^Mg reaction rate, acceptable nucleosynthesis might still be achieved with a cutoff as low as 18M_{sun}_. This would require, however, a supernova frequency three times greater than the fiducial value obtained when all stars explode in order to produce the required ^16^O. The effects of varying M_BH_ on the nucleosynthesis of ^60^Fe and ^26^Al, the production of helium as measured by {Delta}Y/{Delta}Z, and the average masses of compact remnants are also examined. Description: The yield tables of Woosley & Heger (2007PhR...442..269W) give the nucleosynthesis of all species from hydrogen through lead for supernovae resulting from non-rotating massive stars with solar metallicity for the following initial masses: 12-33 (every integer mass), 35-60 (every 5 masses), 60-80 (every 10 masses), 100, and 120 solar masses. The authors calculated explosions for four sets of models parameterized by the mass cut and explosion energy. Here we use their standard set for which the explosion energy was 1.2x10^51^erg and the mass cut was located at the "entropy jump" where S/N_A_k=4.0. These are their "A" models. The values of some key species are provided in Table 1. Using this grid of nucleosynthetic yields, we constructed a stellar population using the high-end initial mass function described by Reid & Wilson (2006ApJ...650..970R). See section 2 for further explanations. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table1.dat 180 64 Yields table for 12<=M/M{sun}<=120 -------------------------------------------------------------------------------- See also: J/A+A/566/A146 : Pair-instability supernovae models (Kozyreva+, 2014) J/A+A/558/A131 : Model spectra of hot stars at the pre-SN stage (Groh+, 2013) J/ApJS/199/38 : Presupernova evolution (Limongi+, 2012) J/ApJ/724/341 : Nucleosynthesis of massive metal-free stars (Heger+, 2010) Byte-by-byte Description of file: table1.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 6 A6 --- Model Model type (1) 8- 10 I3 Msun Mass [12/120] Initial model mass 12- 20 E9.3 Msun H [0/36] The H yield 22- 30 E9.3 Msun He [0.05/64] The He yield 32- 40 E9.3 Msun C [0.002/11] The C yield 42- 50 E9.3 Msun N [0/0.6] The N yield 52- 60 E9.3 Msun O [0.007/8] The O yield 62- 70 E9.3 Msun Ne [0.001/2] The Ne yield 72- 80 E9.3 Msun Mg [0.0007/0.5] The Mg yield 82- 90 E9.3 Msun Si [0.0008/0.5] The Si yield 92-100 E9.3 Msun S [0.0004/0.3] The S yield 102-110 E9.3 Msun Ar [0.0001/0.06] The Ar yield 112-120 E9.3 Msun Ca The Ca yield 122-130 E9.3 Msun Ge70 The ^70^Ge yield 132-140 E9.3 Msun Se76 The ^76^Se yield 142-150 E9.3 Msun Sr86 The ^86^Sr yield 152-160 E9.3 Msun Sr87 The ^87^Sr yield 162-170 E9.3 Msun Al26 The ^26^Al yield 172-180 E9.3 Msun Fe60 The ^60^Fe yield -------------------------------------------------------------------------------- Note (1): Model type (see the "Description" section above): SN = The "A" supernova explosion model (Woosley & Heger 2007PhR...442..269W). pre-SN = The "A" presupernova winds model (Woosley & Heger 2007PhR...442..269W). See the Description section above. -------------------------------------------------------------------------------- History: From electronic version of the journal ================================================================================ (End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 15-Dec-2014