STELLAR MODELS

AGB models	solar model
SAGB models	SAGB Visualisation tool
PMS models	PMS Visualisation tool

Yields from AGB stars experiencing a PIE

When using these data, please refer to :

The intermediate neutron capture process.
III. The i-process in AGB stars of different masses and metallicities without overshoot
Choplin A., Siess L., Goriely S., 2022, A&A, 667, 155

and

The intermediate neutron capture process.
V. The i-process in AGB stars with overshoot
Choplin A., Siess L., Goriely S., 2024, A&A, 684, 206

Available files

elemental yields (mass fraction)	without overshooting	with overshooting
elemental yields [X/Fe]	without overshooting	with overshooting
isotopic yields	without overshooting	with overshooting
initial elemental abundances	without overshooting	with overshooting
initial isotopic abundances	without overshooting	with overshooting

Header description

Each column corresponds to a stellar model whose properties are described in the header (first 12 lines).

The header contains the following information :

ini. mass : initial stellar mass in M_sun
[Fe/H] : initial composition in terms of [Fe/H]
metallicity : initial metallicity Z in mass fraction
ini.compo. : specifies whether the initial composition is solar or alpha-enhanced
f_top : when present, specifies the amount of overshooting at the top of the thermal pulse
npulse : the number of thermal pulses during the AGB phase (pulse declared if T_pulse>200MK)
PIE? : flag to indicate whether the model experiences a PIE or not
final mass : the final stellar mass of the model in M_sun
ej. mass : the total mass ejected in M_sun

The name of the model is written in the 11th line and is the same as in the paper.

Description of yields_el.dat

This file contains the yields for each element. The yields are expressed in mass fraction. They correspond to the mass (in M_sun) of each element ejected by the stellar winds, divided by the total mass ejected by the model (given in the header).

The denominator is equal to the total mass ejected, which is given in the header.

Description of yields_el_ini.dat

Same file as yields_el.dat but here the initial elemental mass fractions are reported.

Description of yields_iso.dat

Same file as yields_el.dat but here the yields in mass fractions are reported for all isotopes.

NOTE : the yield of the isotopes ca40, zn70, ge76, se82, te130, xe136, nd150 and pt192 are not reported for the models without PIE (M1.0z2.0, M2.0z3.0a, M2.0z2.0, M3.0z3.0, M3.0z2.5 and M3.0z2.0). In these models, we used a reduced s-process network of 411 isotopes where these isotopes are not included. These elements are not synthesized by the s-process at low neutron densities and their initial abundance is low except for ca40, whose abundance in the reduced network was added to ca42.

Description of yields_iso.dat

Same file as yields_iso.dat but here the initial isotopic mass fractions are reported.

Super-AGB Yields

SAGB yields for various assumptions concerning the efficiencies of convection and third-dredge-up.

The 5 tables are also available at CDS

Table2	Standard yields (no 3rd dredge-up, λ=0)
Table3	High 3rd dredge-up efficiency yields (λ=0.8)
Table4	Low 3rd dredge-up efficiency yields (λ=0.3)
Table5	High envelope temperature yields (1.1*Tenv)
Table6	Low envelope temperature yields (0.9*Tenv)

Grids of evolutionary models (2010)

Reference to be mentioned:

Siess L. 2010, A&A, 512, A10 PDF

Carolyn Doherty's yields

Yields available for Z=0.02, 0.008, 0.004, 0.001, 0.0001 for various mass loss rates and opacity treatments

Super-AGB Models up to the end of Carbon Burning

Explanation of file variables

Table 1	Z = 0.00001, Y = 0.2479
Table 2	Z = 0.0001, Y = 0.2480
Table 3	Z = 0.001, Y = 0.2492
Table 4	Z = 0.004, Y = 0.2533
Table 5	Z = 0.008, Y = 0.2587
Table 6	Z = 0.020, Y = 0.2748
Table 7	Z = 0.040, Y = 0.3017d
Table 8	Z = 0.0001, Y = 0.2480 + overshooting
Table 9	Z = 0.020, Y = 0.2748 + overshooting
Table00	Complete grid of models (SAGB_all_grids.tgz)

Grids of evolutionary models (2007)

Online article tables

Table 1	models properties prior to C-burning
Table 2	models properties during C-burning
Table 3	surface abundances at the end of 1DUP
Table 4	surface abundances at the end of 2DUP

Initial composition (mass fraction of each element)