Equation of State Sub-Library: Version 0.910
Public Member Functions | Data Fields | Static Public Attributes
oo_eos Class Reference

The EOS tables from O'Connor and Ott. More...

#include <gen_sn_eos.h>

Inheritance diagram for oo_eos:
gen_sn_eos

Detailed Description

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 attribution-noncommercial-share alike license. This O2scl code to read those tables is licensed (along with all O2scl 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 O2scl distribution in doc/o2scl/eos/extras/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
! relativistic-mean 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 low-density 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/deps|rho
! dpdrhoe	   dyn cm^3/cm^2/g   dp/drho|eps
! 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.


Definition at line 500 of file gen_sn_eos.h.

Public Member Functions

virtual void load (std::string fname, size_t mode)
 Load table from filename fname.
virtual void load (std::string fname)
 Load table from filename fname.
virtual void beta_eq_T0 (size_t i, double &nb, double &E_beta, double &P_beta, double &Ye_beta, double &Z_beta, double &A_beta)
 Compute properties of matter in beta equilibrium at zero temperature at a baryon density grid point.

Data Fields

tensor_gridcs2
 Speed of sound in cm^2/s^2.
tensor_griddedt
 C_V in erg/g/K.
tensor_griddpderho
 dpderho in dyn*g/cm^2/erg
tensor_griddpdrhoe
 dpdrhoe in dyn cm^3/cm^2/g
tensor_gridgamma
 Gamma.
tensor_gridmu_e
 Electron chemical potential per baryon including rest mass.
tensor_gridmuhat
 mun - mup
tensor_gridmunu
 mue - mun + mup
ovector rho
 The original mass density grid from the table in g/cm^3.
double energy_shift
 Energy shift for table storage in erg/g.

Static Public Attributes

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.

Member Function Documentation

virtual void oo_eos::beta_eq_T0 ( size_t  i,
double &  nb,
double &  E_beta,
double &  P_beta,
double &  Ye_beta,
double &  Z_beta,
double &  A_beta 
) [inline, virtual]

This EOS table doesn't have T=0 results, so we extrapolate from the two low-temperature grid points.

Implements gen_sn_eos.

Definition at line 556 of file gen_sn_eos.h.


The documentation for this class was generated from the following file:
 All Data Structures Namespaces Files Functions Variables Typedefs Enumerations Friends

Documentation generated with Doxygen. Provided under the GNU Free Documentation License (see License Information).

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