Class eos_sn_stos (o2scl)¶

class eos_sn_stos : public o2scl::eos_sn_base¶
The H. Shen et al. supernova EOS.
This class is experimental.
In order to force the EOS to a uniform grid, linear interpolation is used to recast the variation in baryon density, choosing the grid in baryon density to be the same as the section in the table with T=0.1 MeV and \( Y_p = 0.1 \) for all temperature and proton fraction points.
The data for eos_sn_base::E, eos_sn_base::F, eos_sn_base::S, and eos_sn_base::P is not stored in the table but can be computed with eos_sn_base::compute_eg().
See also the documentation at ref eos_sn_base and the general description in the Finitetemperature Equation of State Tables section of the User’s guide.
See also [Shen98] and [Shen98b].
Todo
In class eos_sn_stos: Add the T=0 and Ye=0 data to this class. Separate tables for these cases have been released, but I don’t think this class can read them yet.
Note
Does not contain the EOS, only provides some code to manipulate it. This class is designed to be used with the file which was originally called
eos.tab
and now referred to aseos1.tab
and stored e.g. at http://user.numazuct.ac.jp/~sumi/eos/.Note
Thanks to Matthias Hempel for providing the correct temperature grid.
Additional data included in this EOS

tensor_grid3 &log_rho¶
Logarithm of baryon number density in \( \mathrm{g}/\mathrm{cm}^3 \).

tensor_grid3 &nB¶
Baryon number density in \( \mathrm{fm}^{3} \).

tensor_grid3 &log_Y¶
Logarithm of proton fraction.

tensor_grid3 &Yp¶
Proton fraction.

tensor_grid3 &M_star¶
Nucleon effective mass in MeV.

tensor_grid3 &quark_frac¶
Fraction of quark matter.

static const size_t orig_mode = 0¶

static const size_t quark_mode = 1¶

static const size_t fyss_mode = 2¶

inline eos_sn_stos()¶

virtual void load(std::string fname, size_t mode)¶
Load table from filename
fname
with modemode
.

virtual void load_auto(std::string model, std::string directory)¶
Look for EOS table for model
model
in directorydirectory
and download from cloud storage if not found.