Can the pressure be made to match more closely?
Convert to a o2scl::eos_had_base object and offer an associated interface?
There might be room to improve the testing of the finite temperature part a bit.
There is some repetition between calc_e() and calc_temp_e() that possibly could be removed.
Include the analytic relations from Constantinou et al.
Replace fmsom() with f_effm_scalar(). This has to wait until f_effm_scalar() has a sensible definition when mn is not equal to mp
Could write a function to compute the "symmetry free energy" or the "symmetry entropy"
Compute the speed of sound or the number susceptibilities?
A lot of the numerical derivatives here might possibly request negative number densities for the nucleons, which may cause exceptions, espescially at very low densities. Since the default EOS objects are GSL derivatives, one can get around these issues by setting the GSL derivative object step size, but this is a temporary solution.
calc_temp_p()
at very low densities. I have had problems, for example, with mun=5.0, mup=6.5
at T=1.0/197.33
. Storage in a o2scl::table object isn't necessary, and storing in a vector object is more efficient.
Allow the pressure to be specified to make the EOS more accurate?
There is a bit of duplication between calc_density_noneq() and calc_density_fixnp() which could be streamlined.
Add fermion and boson statistics to the nuclei in the distribution.
This class internally mixes ubvector, ubmatrix, gsl_vector and gsl_matrix objects in a confusing and non-optimal way. Fix this.
Allow user to change derivative object? This isn't possible right now because the stepsize parameter of the derivative object is used.
Add option to rescale energies and chemical potentials to different masses.
Create a o2scl::table object, possibly using tensor_grid::vector_slice.
Show how matrix_slice and vector_slice can be used with this object.
Add option to load and store a separate lepton/photon EOS
Add pions?
Create a standard output format? Output to stellarcollapse.org HDF5 format?
Warn if the EOS becomes pure neutron matter.
Some of the auxillary quantities can be computed directly without using the table methods and the EOS calculation would be a bit faster.
Make a GSL-like set() function
Rework EOS interface and implement better integration with the other O2scl_eos EOSs.
Remove the unit-indexed arrays.
Try moving some of the storage to the heap?
Some of the arrays seem larger than necessary.
The function o2scl::nstar_rot::new_search() is inefficient because it has to handle the boundary conditions separately. This could be improved.
Make the solvers more robust. The ang_vel() and ang_vel_alt() functions appear particularly unstable.
Sort energy levels at the end by energy
Improve the numerical methods
Make the neutron and proton orbitals more configurable
Generalize to .
Allow more freedom in the integrations
Consider converting everything to inverse fermis.
Convert to zero-indexed arrays (mostly done)
Warn when the level ordering is wrong, and unoccupied levels are lower energy than occupied levels
Connect with o2scl::nucmass ?
Add translational energy?
Remove excluded volume correction and compute nuclear mass relative to the gas rather than relative to the vacuum.
In principle, Tc should be self-consistently determined from the EOS.
Does this work if the nucleus is "inside-out"?
non_interacting
for the particle inputs. This is not very graceful...Documentation generated with Doxygen. Provided under the
GNU Free Documentation License (see License Information).