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Ideas for Future Development
Class o2scl::eos_crust

Can the pressure be made to match more closely?

Convert to a o2scl::eos_had_base object and offer an associated interface?

Class o2scl::eos_had_apr

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.

Global o2scl::eos_had_apr::parent_method
This variable is probably unnecessary, as the syntax
eos_had_apr apr;
ccout << apr.eos_had_base::fcomp(0.16) << endl;
works just as well.
Class o2scl::eos_had_base

Could write a function to compute the "symmetry free energy" or the "symmetry entropy"

Compute the speed of sound or the number susceptibilities?

Compute isoscalar and isovector effective masses

Global o2scl::eos_had_base::saturation ()
It would be great to provide numerical uncertainties in the saturation properties.
Class o2scl::eos_had_ddc
Implement the finite temperature EOS properly.
Class o2scl::eos_had_potential
Calculate the chemical potentials analytically
Class o2scl::eos_had_rmf
  • Finish putting the err_nonconv system into calc_p(), calc_temp_e() and fix_saturation(), etc.
  • It might be nice to remove explicit reference to the meson masses in functions which only compute nuclear matter since they are unnecessary. This might, however, demand redefining some of the couplings.
  • Fix calc_p() to be better at guessing
  • The number of couplings is getting large, maybe new organization is required.
  • Overload eos_had_base::fcomp() with an exact version
  • It would be nice to analytically compute the Jacobian of the field equations for the solver
Global o2scl::eos_had_rmf::calc_e (fermion &ne, fermion &pr, thermo &lth)
Improve the operation of this function when the proton density is zero.
Global o2scl::eos_had_rmf::calc_eq_p (fermion &neu, fermion &p, double sig, double ome, double rho, double &f1, double &f2, double &f3, thermo &th)
Probably best to have f1, f2, and f3 scaled in some sensible way, i.e. scaled to the fields?
Global o2scl::eos_had_rmf::calc_p (fermion &ne, fermion &pr, thermo &lth)
It may be possible to make the solver for the field equations more robust
Global o2scl::eos_had_rmf::n_charge
Should use eos_had_base::proton_frac instead?
Class o2scl::eos_had_rmf_delta
Finish the finite temperature EOS
Class o2scl::eos_had_skyrme
  • There is some code duplication between calc_e() and calc_temp_e() which could be simplified.
Class o2scl::eos_nse
Right now calc_density() needs a very good guess. This could be fixed, probably by solving for the log(mu/T) instead of mu.
Class o2scl::eos_quark_cfl

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.

Class o2scl::eos_sn_base

Currently, tensor_grid objects are based on ublas vectors and thus require a copy for HDF5 output. Can tensor_grid objects be based on std::vector instead?

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?

Class o2scl::eos_sn_oo
Loading an EOS currently requires loading the HDF5 file and then copying it. This wouldn't be necessary if the O2scl tensor had the same ordering as the indices in the original HDF5 file.
Class o2scl::eos_tov_buchdahl
Figure out what to do with the buchfun() function
Class o2scl::nstar_cold
Warn if the EOS becomes pure neutron matter.
Class o2scl::nucleus_rmf

Sort energy levels at the end by energy

Improve the numerical methods

Make the neutron and proton orbitals more configurable

Generalize to $ m_n \neq m_p $ .

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 ?

Class o2scl::nucmass_ldrop_skin

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"?

Global o2scl::tov_solve::min_log_pres
Replace this with the proper value from std::limits?
Page Other Todos
Right now, the equation of state classes depend on the user to input the correct value of non_interacting for the particle inputs. This is not very graceful...

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