(Website under construction.)
Currently models starting from four different progenitors are available. The progenitors are s9.0 from Woosley and Heger (2015), s18.6 and s27.0 from Woosley et al. (2002), s20 from Woosley and Heger (2007), and s18.8 from Sukhbold et al. (2018). The progenitor and the time chosen to trigger the explosion determine the resulting baryonic neutron star mass of a model. Currently models with baryonic neutron star mass of 1.36, 1.44, 1.62, 1.77, and 1.93 solar masses are available. Furthermore, the models differ in the choice of the hadronic equation of state in the high-density regime. Currently models with the following equation of state tables are available: DD2 (Typel et al. 2010), LS220 (Lattimer and Swesty 1991), SFHo and SFHx (Steiner et al. 2013). Standard models include the effects of both muons (hence with six neutrino species) and convection. But we also provide models without muons (hence with four neutrino species) or without convection. These models are marked by an appended -m (without muons) or -c (without convection) in the modelname and filename. E.g. the model 1.62DD2-m has a baryonic neutron star mass of approximately 1.62 solar masses, uses the DD2-EoS, and was calculated with convection but without muons.
Neutrino Luminosities Neutrino Signals Radial Neutrino Moment Profiles Radial Hydro Profiles Fiorillo et al. (2023): Supernova Simulations Confront SN 1987A Neutrinos