Equations of State of Hadronic Matter

O2scl_eos

The hadronic equations of state are all inherited from eos_had_base : eos_had_schematic, eos_had_skyrme, eos_had_rmf, eos_had_apr, and eos_had_potential.

The eos_had_base class includes several methods that can be used to calculate the saturation properties of nuclear matter. These methods are sometimes overloaded in descendants when exact formulas are available.

There is also a set of classes to modify the quartic term of the symmetry energy: eos_had_sym4_rmf, eos_had_sym4_apr, eos_had_sym4_skyrme, and eos_had_sym4_mdi all based on eos_had_sym4_base which can be used in eos_had_sym4.

Akmal-Pandharipande-Ravenhall EOS example

This example computes the APR EOS with eos_had_apr. It computes nuclear and neutron matter and then matter in beta-equilibrium with both a Maxwell construction (as done in the [Akmal98eo]) and a Gibbs construction to match the low- and high-density phases. Afterwards it computes the properties of neutron stars from the EOS. Most of the data is stored in table_units objects and then written to HDF files in the examples directory.

This example is rather lengthy and the full source code is not duplicated here. The class created in that example is documented at ex_eos_had_apr . The EOS and mass radius curves for APR created by this example and for the Skyrme model SLy4 from the next example is below. The third figure below is the Gibbs phase transition for APR.

_images/ex_eos_had_eos.png _images/ex_eos_had_mvsr.png _images/ex_eos_had_gibbs.png

Typical output:

Skyrme EOS example

This example computes the EOS and neutron star properties using eos_had_skyrme from a Skyrme model.

This example is rather lengthy and the full source code is not duplicated here. The class created in that example is documented at ex_eos_had_skyrme .

Typical output: