Yield References - arsenal-popsynth/arsenal_gear GitHub Wiki

It seems like a decent database of yields was compiled as part of Chempy so that will be good to take a look at.

NuGrid

Yields are available for vast majority of interesting elements (and isotopes) tabulated for masses $[1, 1.65, 2, 3, 4, 5, 6, 7, 12, 15, 20, 25],M_{\odot}$ and metallicities $[0.02, 0.01, 0.006, 0.001, 0.0001]$. Also includes other interesting features, e.g., super-AGB and accreting white dwarfs.

Tables available at https://nugrid.github.io/content/data.

Release papers:

Pignatari et al. (2016): GB and massive stars for metallicities Z = 0.02, 0.01.
Ritter et al. (2018): Adds Z = 0.006, 0.001, 0.0001. More masses at all metallicities. All models computed with MESA.
Battino et al. (2019), Battino et al. (2021): Low-mass AGB model update for 2 and 3 Msun using for existing metallicities Z = 0.02, 0.01, 0.001, and adding Z = 0.03, 0.002.
Jones et al. (2016): Super-AGB evolution with H ingestion into the He-burning convection zones.
Lawson et al. (2022): Radioactive isotopes from analysis of 62 core-collapse models
Stephens et al. (2021): H ingestion into convective He shell for rapidly accreting white dwarfs.

Modelling details:

Stellar Evolution: Treated using 1D models MESA Paxton et al. (2011), with earlier yield sets also using GENEC models Eggenberger et al. (2008).
Nucleosynthesis: Performed in post-process using temperature, density, and diffusion coefficients stored at every time-step of the 1D stellar evolution models.
Pre-SNe winds: Mass-loss prescription of massive stars ($\geq12,{\rm M}{\odot}$) depends on effective temperature and surface hydrogen mass fraction. Adopts models from Vink et al. (2001) for $T{\rm eff} > 1.1\times10^{4},{\rm K}$ and transitions to de Jager et al. (1988) at lower temperatures (10^{4},{\rm K}). Different models adapted at low hydrogen mass fraction ($X_H<0.4$). Rates depend explicitly on metallicity and correction factor of 0.8 is applied for MS OB stars, see Ritter et al. (2018) for details.
Supernovae: Nuclear yields are derived by applying the nucleosynthesis network to semi-analytic models for SNe evolution following Fryer et al. (2012). Two explosions energies are considered (labeled rapid and delay). Rapid produce smaller remnants in general, but fails to drive explosions for the most massive stars (resulting in larger remnant). Shock velocities determined by Sedov solution, assuming strong shock limit (Chevalier 1989) to compute density and temperature. Model produce similar results to Woosley & Weaver (1995).
Giant branch: Mass loss rates follow prescriptions from Reimers (1975) for red giant brach and Blöcker (1995) for AGB phase.
Super AGB:

Limongi & Chieffi (2018)

Include yields majority of elements (and isotopes) for massive stars [ 13, 15, 20, 25, 30, 40, 60, 80, 120] ${\rm M}_{\odot}$, with initial iron abundance ([Fe/H]) [0, -1, -2, -3], and three different models for stellar rotation [0, 150, 300] km/s.

Yields available at http://orfeo.iaps.inaf.it/

Release paper: Limongi & Chieffi (2018)

Stellar evolution: Treated using the FRANEC stellar evolution code, a 1D evolutionary code introducing the average thermal and mechanical distortions as a result of stellar rotation. Initial He abundance is determined from current solar values. Mixing efficiency is calibrated through fitting $v \sin(i)$ and surface N abundance to stars in LMC open cluster NGC 2004. See Limongi & Chieffi (2018) for details.
Winds from OB stars: Mass loss rates adopts models from Vink (2000, 2001) for Blue Super Giant ($T_{\rm eff} > 12,000,{\rm K}$), de Jager et al. (1988) for Red Super Giant ($T_{\rm eff} <> 12,000,{\rm K}$), and Nugis & Lamers (2000) for Wolf-Rayet phase. Mass loss is enhanced in rotating models, following Heger et al. (2000).
Core-collapse SNe: The recommended set of yields is calibrated by assuming that stars eject $0.07,{\rm M}{\odot}$ of $^{56}\rm Ni$ unless undergoing direct collapse to black hole (stellar mass $>25,{\rm M}{\odot}$).

Seitenzahl et al. (2013)

Yields from SNe type Ia, including metallicity dependence [0.01, 0.1, 0.5, 1.0] ${\rm Z}_{\odot}$.

Tables available through tables in publication.

Release paper: Seitenzahl et al. (2013)

Type Ia SNe: Modelled using 3D hydrodynamical simulations of explosions for Chandrasekhar-mass delayed-detonation models. Includes stochastic modelling of initial detonation location based on turbulent velocity fluctuations and fuel density.