Class eos_sn_oo (o2scl)¶

class eos_sn_oo : public o2scl::eos_sn_base¶
The EOS tables from O’Connor and Ott.
This class reads the HDF5 EOS tables generated by E. O’Connor and C. Ott in [OConnor10]. The tables are available from
http://stellarcollapse.org/equationofstate
and are available under a creative commons attributionnoncommercialshare alike license. This code to read those tables is licensed (along with all code) under the GPLv3 license (with permission from Evan O’Connor).
The original README file from O’Connor and Ott’s EOSdriver code is available in the distribution in
doc/o2scl/eos/sphinx/static/scollapse_README
and is reproduced below! ######################################################### ! ! Copyright C. D. Ott and E. O'Connor, July 2009 ! ! ! ! EOS constructed on the basis of the Shen et al. 1998 ! relativisticmean field nuclear EOS table. Electrons (fully ! general, based on TimmesEOS) and Photons added. ! ! Original Shen EOS table extent: ! ! Density: 10^5.1 to 10^15.4 g/cm^3 ! Temperature: 0.1 to 100 MeV ! Ye: 0.01 to 0.56 ! ! Table extent of current table ! (myshen_test_220r_180t_50y_extT_20090312.h5) ! ! Density: 10^3 to 10^15.36 g/cm^3 ! Temperature: 0.01 to 250 MeV ! Ye: 0.015 to 0.56 MeV ! ! This bigger table is realized by extending the ! original Shen table in multiple ways in multiple ! directions: ! ! (a) density: ! Match of pure ideal gas of Ni56 + electrons/positrons + ! photons at densities below 10^7 g/ccm  at this density ! pressures, energies and entropies match okayish with the ! values in the Shen table. The compositions (A,Z,xh,xa,xp,xn) ! are kept constant in the lowdensity region and n and p ! chemical potentials are set to 0. !  ideally, at low densities, a full NSE EOS with nuclear ! reaction network (at low T) should be stiched onto the ! Shen; working on that, but not yet ready. ! ! (b) temperature (extrapolation): ! At high density: linear extrapolation of everything in T to lower ! temperatures and higher temperatures. At low densities (below 10^7 ! g/ccm), ideal gas of Ni56 + electrons/positrons + photons. ! ! ! Variable Units Description ! pointsrho dimensionless number of table points ! in log_10(rho) ! pointstemp dimensionless number of table points ! in log_10(temp) ! pointsye dimensionless number of table point in Y_e ! logrho log10(rho) index variable rho ! logtemp log10(MeV) index variable temperature ! ye number fraction index variable electron fraction ! Abar A average heavy nucleus A ! Zbar Z average heavy nucleus Z ! Xa number fraction alpha particle number frac ! Xh number fraction heavy nucleos number frac ! Xn number fraction neutron number frac ! Xn number fraction proton number frac ! cs2 cm^2/s^2 speed of sound squared ! dedt erg/g/K C_v ! dpderho dyn g/cm^2/erg dp/depsrho ! dpdrhoe dyn cm^3/cm^2/g dp/drhoeps ! energy_shift erg/g Energy shift for table storage ! entropy k_B/baryon specific entropy ! gamma dimensionless Gamma_1 ! logenergy log10(erg/g) specific internal energy ! logpress log10(dyn/cm^2) pressure ! mu_e MeV/baryon electron chemical potential ! INCLUDING electron rest mass ! mu_p MeV/baryon proton chemical potential ! mu_n MeV/baryon neutron chemical potential ! muhat MeV/baryon mu_n  mu_p ! munu MeV/baryon mu_e  mun + mu_p ! ! ! * energy shift: ! ! In some regions the negative nuclear binding energy ! is larger in magnitude than the thermal/excitation energy. In this ! case the specific internal energy (eps) becomes negative. To allow for ! storage and interpolation of eps in logarithmic fashion, the energy ! is shifted up by an energy shift specified in the variable "energy_shift". ! This energy shift is handled internally in the EOS routines.
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.
 Idea for Future:
Loading an EOS currently requires loading the HDF5 file and then copying it. This wouldn’t be necessary if the tensor had the same ordering as the indices in the original HDF5 file.
Additional data included in this EOS

tensor_grid3 &cs2¶
Speed of sound in cm^2/s^2.

tensor_grid3 &dedt¶
C_V in erg/g/K.

tensor_grid3 &dpderho¶
dpderho in dyn*g/cm^2/erg

tensor_grid3 &dpdrhoe¶
dpdrhoe in dyn cm^3/cm^2/g

tensor_grid3 &gamma¶
Gamma.

tensor_grid3 &mu_e¶
Electron chemical potential per baryon including rest mass.

tensor_grid3 &muhat¶
mun  mup

tensor_grid3 &munu¶
mue  mun + mup

tensor_grid3 &XHe3¶
Helion fraction.

tensor_grid3 &XLi4¶
Lithium4 fraction.

tensor_grid3 &Xt¶
Triton fraction.

tensor_grid3 &Xd¶
Deuteron fraction.

std::vector<double> rho¶
The original mass density grid from the table in g/cm^3.

double energy_shift¶
Energy shift for table storage in erg/g.
Table modes

static const size_t ls_mode = 0¶
Use the J. Lattimer et al. method for handling the chemical potentials.

static const size_t stos_mode = 1¶
Use the H. Shen et al. method for handling the chemical potentials.

static const size_t hfsl_mode = 2¶
Set for a Hempel et al. table with light nuclei.

static const size_t sht_mode = 3¶
Set for a G. Shen et al. table.

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.
Public Functions

inline eos_sn_oo()¶