A simple supernova model

The Agile-IDSA code provides tools to run a rudimentary and approximate model of a core-collapse supernova with neutrino transport in spherical symmetry through the phases of stellar collapse, bounce, and early postbounce evolution. The code is not fool-proof, requires undocumented customisation to the local computational infrastructure, and is meant for people who work, or get started to work, in the field of supernova theory. Of course we are pleased if Agile-IDSA turns out to be useful also for investigators of supernova input physics, or if parts of the code can be extended to broader astrophysical application.

The separate hydrodynamics part Agile (Adaptive Grid with Implicit Leap Extrapolation) has been used in general relativistic spherically symmetric models of stellar core collapse and postbounce evolution with Boltzmann neutrino transport (e.g. Liebendörfer et al. 2004, ApJS 150, 263), while the neutrino transport part based on the isotropic diffusion source approximation (IDSA) has been used in multidimensional models of stellar core collapse and postbounce evolution (e.g. Whitehouse & Liebendörfer 2008, PoS(NIC X)243; Suwa et al. 2011, ApJ 738, 165, Cabezo et al., A&A 619A.118C, 2018). Here we put the two pieces together to a standalone and physically simple spherically symmetric supernova model and possible toolkit for further projects. The code implements physics outlined in the following publications: Hydrodynamics: 

Liebendörfer, Rosswog & Thielemann 2002, ApJS 141, 229. 
Neutrino parameterisation: Liebendörfer 2005, ApJ 633, 1042. 
Neutrino transport: Liebendörfer, Whitehouse & Fischer 2009, ApJ 698, 1174. 
Weak interactions: Mezzacappa & Bruenn 1993, ApJ 405, 637. 
Equation of state: Lattimer & Swesty 1991, Nuc. Phys. A 535, 331. K=220 MeV.

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Current version: agile-idsa_140620.zip. Agile-IDSA is subject to the GNU General Public License as published by the Free Software Foundation (version 3 or later). 

Acknowledgement

This project was mainly funded by the Swiss National Science Foundation under grant No 20-47252.96, 20-53798.98, PP002-106627/1, PP00P2_124879/1 and the High Performance and High Productivity Computing (HP2C) initiative http://www.hp2c.ch. We equally acknowledge the stimulating and supportive research-environment at the Canadian Institute for Theoretical Astrophysics in Toronto and within the ESF Research Networking Programme 'CompStar'.\

This file datafiles.zip contains output data from a comparison between two independently developed supernova codes which solve the Boltzmann neutrino transport equation (Agile-Boltztran of the Oak Ridge/Basel group and Vertex of the Munich group). The data is described and published in Liebendoerfer, Rampp, Janka, & Mezzacappa 2005, ApJ, 620, 840.

There are not many equations of state that describe matter in a broad density range for finite temperatures (e.g. Lattimer-Swesty, Shen et al.). Many hydrodynamics codes prefer the equation of state in a tabular form. As it can be quite time consuming to convert the interactive Lattimer-Swesty equation of state version 2.7 to a table, we share here our eos_module.f eostable.zip that builds a table with the LSEOS v2.7 and performs interpolations. Although it is not meant to be especially accurate, efficient, or sophisticated, it may be a starting point and ease the transition from polytropic equations of state to a microphysical equation of state.