Hi All,
later today, we will merge the current development branch with the trunk branch of GRHydro.
Major changes:
* GRHydro now knows about electron fraction and temperature and can handle finite-temperature EOS. In order to use this feature, you have to set: hydrobase::temperature_evolution_method = "GRHydro" and hydrobase::y_e_evolution_method = "GRHydro". In addition, you'll of course need a hot EOS (see below) and appropriate initial data.
* GRHydro now uses EOS_Omni. The EOS_Base dependence has been removed. You will need to change your parameter files and activate EOS_Omni which will be moved to the EinsteinEOS arrangement today. Example parameters for a TOV NS evolution are: eos_omni::poly_gamma = 2.0 eos_omni::poly_gamma_ini = 2.0 eos_omni::poly_k = 100.0 eos_omni::gl_gamma = 2.0 eos_omni::gl_k = 2.0
EOS_Omni currently supports a polytropic EOS, a gamma-law EOS (this is what we used to call "ideal fluid" EOS), a hybrid EOS (a hot 2-piece polytrope), and nuc_eos, which can handle hot tabulated EOS. Tables for the latter can be obtained from http://www.stellarcollapse.org/microphysics. This currently works well for core collapse, but has not been tried for NS evolutions. When using the nuc_eos routines, please make reference to http://iopscience.iop.org/0264-9381/27/11/114103 .
* GRHydro currently still supports the second legacy EOS interface "EOSG_Base", but this support will be removed soon to simplify the code.
Please let me and Frank Loeffler know if you have any concerns about the above.
Best,
- Christian Ott for the Einstein Toolkit maintainers.