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 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:
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FileName Lrecl Records Explanations
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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
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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
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Bytes Format Units Label Explanations
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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 λdup defined by Goriely & Mowlavi
(2000A&A...362..599G 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
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Note (1): λdup=λ*(DMh/Mcsh) where Mcsh is the maximum mass
of the intershell convection zone.
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Byte-by-byte Description of file: tablea[23456].dat
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Bytes Format Units Label Explanations
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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))
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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.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 04-Oct-2010