J/MNRAS/403/1413 Updated stellar yields from AGB models (Karakas, 2010)
Updated stellar yields from asymptotic giant branch models. Karakas A.I. <Mon. Not. R. Astron. Soc., 403, 1413-1425 (2010)> =2010MNRAS.403.1413K
ADC_Keywords: Models ; Stars, giant ; Abundances Keywords: nuclear reactions, nucleosynthesis, abundances - stars: AGB and post-AGB - stars: Population II - ISM: abundances Abstract: An updated grid of stellar yields for low- to intermediate-mass thermally pulsing asymptotic giant branch (AGB) stars is presented. The models cover a range in metallicity Z=0.02, 0.008, 0.004 and 0.0001, and masses between 1 and 6M☉. New intermediate-mass (M≥3M☉) Z=0.0001 AGB models are also presented, along with a finer mass grid than used in previous studies. The yields are computed using an updated reaction rate network that includes the latest NeNa and MgAl proton capture rates. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tablea1.dat 241 727 Structural information from the new AGB models tablea2.dat 123 1232 The stellar yields for the Z = 0.02 model tablea3.dat 123 1155 The stellar yields for the Z = 0.008 model tablea4.dat 123 1155 The stellar yields for the Z = 0.004 model tablea5.dat 123 1232 The stellar yields for the Z = 0.0001 model tablea6.dat 123 308 The stellar yields for the models with partial mixing zones
See also: J/A+AS/107/445 : Envelopes of oxygen-rich AGB stars (Hashimoto, 1994) J/ApJS/92/125 : Post-AGB evolution (Vassiliadis+, 1994) J/A+AS/126/39 : Models of circumstellar dust shells (Steffen+ 1997) J/A+A/512/A10 : Evolution of massive AGB stars. III. (Siess, 2010) Byte-by-byte Description of file: tablea1.dat
Bytes Format Units Label Explanations
1- 4 F4.2 solMass M0 [1/6] Initial mass 6- 11 F6.4 --- Z0 Initial metallicity (0.0200, 0.0080, 0.0040, 0.0001) 13- 16 I4 --- Pulse Pulse number 20- 31 E12.7 solMass Mcore Core mass 34- 45 E12.7 solMass Mcsh Maximum mass of the intershell convection zone 48- 59 E12.7 yr tcsh Duration of intershell convection 62- 73 E12.7 solMass Ddredge Mass dredged into the envelope 76- 87 E12.7 --- lam Extent of the partial mixing zone, lambda 90-101 E12.7 --- lam.dup lambdadup defined by Goriely & Mowlavi (2000A&A...362..599G) (1) 104-115 E12.7 K T(He-sh) Maximum temperature in the He-shell 118-129 E12.7 K Tbce Maximum temperature at the base of the convective envelope during the previous interpulse period 132-143 E12.7 K T(H-sh) Maximum temperature in the H-shell during the previous interpulse period 146-157 E12.7 yr iPulse Interpulse period (note that the first entry is set to zero) 160-171 E12.7 solMass Mtot Total mass 174-185 E12.7 solLum Lmax Maximum radiated luminosity during the previous interpulse period 188-199 E12.7 solLum LHe.max Maximum He-luminosity during a thermal pulse 202-213 E12.7 solRad Rmax Maximum stellar radius during the previous interpulse period 215-227 E13.8 mag Mbol Bolometric magnitude 230-241 E12.7 K Teff Effective temperature
Note (1): λdup=λ*(DMh/Mcsh) where Mcsh is the maximum mass of the intershell convection zone.
Byte-by-byte Description of file: tablea.dat
Bytes Format Units Label Explanations
1- 4 F4.2 solMass M0 [1/6.5] Initial mass 6- 11 F6.4 --- Z0 Initial metallicity 13- 17 F5.3 solMass M1 Final mass (1) 22- 25 A4 --- El Species i (2) 31- 32 I2 --- A Atomic mass of the species i 35- 48 E14.9 solMass Yield Net yield 50- 63 E14.9 solMass M(i)lost Mass of species i lost in the wind 65- 78 E14.9 solMass M(i)0 Mass of species i initially present in the wind 80- 93 E14.9 --- <X(i)> Average abundance of species i in the wind (mass fraction) 95-108 E14.9 --- X0(i) initial mass fraction of species i (mass fraction) 110-123 E14.9 --- f Production factor, f=log10(<X(i)>/X0(i))
Note (1): For (M0, Z0, M1): * 6.00 0.0001 1.008: Reimer's mass loss * 6.00 0.0001 1.006: VW93 mass loss * 3.00 0.0200 0.682: partial mixing zone = 2x10-3M☉ * 3.00 0.0080 0.694: partial mixing zone = 2x10-3M☉ * 3.00 0.0040 0.731: partial mixing zone = 2x10-3M☉ * 2.00 0.0001 0.685: partial mixing zone = 2x10-3M☉ Note (2): g represents the sum of abundances from 64Ni to Bi; an increase in g indicates that neutron captures have occurred beyond the end of the network.
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 04-Oct-2010
|The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line|