Department of Theoretical Astrophysics 
Note:
conductivities have been last updated in 2021 A summary of the updates since 2006 is given below. 
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Introduction
Electrical and thermal conductivities of dense plasmas under conditions which take place in the stars have been studied by large number of authors over the twentieth century. Milestones on the theoretical investigation are the classical works by R. E. Marshak (1940), T. D. Lee (1950), J. M. Ziman (1960), L. Spitzer (1962), W. B. Hubbard & M. Lampe (1966  1969), E. Flowers & N. Itoh (1970s). In 80s  90s, significant progress was due to L. Hernquist, N. Itoh, R. Redmer, and their coworkers, as well as other theoretical groups. It would be impossible to give the appropriate credit to all of them in this short introductory note. We restrict ourselves to a brief account only of the results obtained at the Department of Theoretical Astrophysics (DTA) of the Ioffe Institute since late 70s, which are implemented in the Fortran codes presented at this site.
As early as in 1980 Yakovlev and Urpin [1,2] critically analyzed previously published results and presented simple analytic approximations to the conductivities of degenerate electrons dominated by their scattering off ions (in the ion liquid) or off phonons or charged lattice impurities (in the ion crystal). Subsequent more detailed studies of this research team [36], as well as other ones, have confirmed reliability of these results in the range of plasma parameters typical for the thermalinsulating envelopes of cooling neutron stars (at densities of order 10^{3}10^{10} g/cc and temperatures T about 10^{6}10^{9} K, or more precisely, where T is much lower than the electron degeneracy temperature, but not much lower than the ion plasma temperature). At the same time, those later studies have extended the range of considered parameters to lower temperatures [3] at which quantization of ionic motion is important (which is relevant for interiors of cool white dwarfs), to lower density [4] (for outermost layers of neutron stars), and to higher densities (in the inner envelopes of neutron stars) at which the finite nuclear sizes are nonnegligible [6].
Although transport properties of dense stellar plasma are mainly determined by electronion collisions, electronelectron collisions may also be significant for thermal conductivity under certain conditions. The collisions between degenerate electrons have been considered in [1]. They are unimportant if the ions are highly charged or electron degeneracy is strong. Both electronion and electronelectron collisions are taken into acount in the Fortran programs presented at this site.
Electrical and thermal conductivity tensors, as well as thermopower tensor, in strong magnetic fields  the fields in which the electron gyrofrequency is larger than the typical collision frequency  were studied first for the nonquantizing [7] and then for quantizing fields. Kaminker & Yakovlev [8] considered the electron transport across the field and Yakovlev [9] the transport along the field (strongly or weakly quantizing, for arbitrary relativism of the electron gas) as reviewed in Ref.[10]. The results [9] based on the electron distribution function formalism have been confirmed later [11,12] using a more general formalism of electron density matrix.
Recent progress in the treatment of electrical and thermal conductivities of strongly coupled Coulomb plasmas is connected with improvements of ion structure factors relevant to calculation of electron relaxation times. Physics of these improvements has been explained in Ref.[13], and the resulting impact on nonmagnetic conductivities has been explored in Ref.[14]. In the solid phase, multiphonon electron scattering (neglected previously) has been taken into account. In the Coulomb liquid, an approximate treatment has been proposed to describe reduction of the effective electronion collision rate due to incipient ordering of the ions in the regime of strong ion coupling. Both modifications (in the solid and liquid phases) change the kinetic coefficients near the melting point and drastically reduce their discontinuities at the solid/liquid phase interface. Simple analytic approximations for effective relaxation times determined by the electronion and electronelectron collisions in degenerate, fully ionized plasmas have been also published [14].
In Ref.[15], these theoretical advances have been employed to calculate longitudinal, transverse, and Hall components of tensors of electron electrical and thermal conductivities and thermopower in arbitrary magnetic fields. Fitting formulae have been devised and implemented in a Fortran code which is available on these Web pages.
The generalization of the formulae obtained in Ref.[14] to the case where the size of the ions must be taken into account, which is the case for the inner crust of a neutron star (at densities above 10^{11} g/cc), has been given in the Appendix to Ref.[16].
The electronelectron scattering does not contribute in the electrical conductivity, but it can be important for the thermal conductivity. This scattering has been considered by Urpin & Yakovlev [1] and used in Ref.[14]. However, Shternin & Yakovlev [17] reconsidered this mechanism, taking into account Landau damping of transverse plasmons. This effect (neglected before) is due to the difference of the components of the polarizability tensor, responsible for screening the chargecharge and currentcurrent interactions (i.e., different screening of the timelike and spacelike components of the electron currents in the interaction matrix element in quantum electrodynamics). Shternin & Yakovlev found that the Landau damping of transverse plasmons strongly increases the effective electronelectron collision frequency at high densities (where degenerate electrons are relativistic), compared to the older results of Flowers & Itoh and Urpin & Yakovlev. In Ref.[18], a fitting formula has been presented, which reproduces Shternin & Yakovlev results for strongly degenerate plasmas and Hubbard & Lampe ones for weakly or nondegenerate matter.
Chugunov & Haensel [19] considered an alternative heat transport by the plasma ions (phonons) and presented fitting formulae for effective Coulomb logarithms describing scattering of ions off ions and electrons in dense plasmas. (However, by default, we do not use their fit in the latest version of our code, because this correction is, as a rule, unimportant, while its use may cause certain problems.)
Chugunov [20] has shown that the "freezingout" of the Umklapp processes is ineffective in star conditions of degenerate stellar plasmas. This result is now taken into account (see the list of updates below).
Blouin et al. [21] suggested that our formulas underestimate the conductivities around the transition from nondegenerate to strongly degenerate plasmas, which is substantial in the case where the electronelectron scattering is important, viz. for light elements (especially H and He). Cassisi et al. [22] discussed theoretical uncertainties in this region and suggested alternative ways to bridge the domains of nondegenerate and strongly degenerate plasmas, which are now implemented in the code on the present site.
To summarize, the numerical data and Fortran programs at our Web site are based on the theoretical results published in Refs.[1418, 20, 22]. The plasma is assumed fully ionized (collisions with neutrals are neglected). This model may be still useful for evaluation of conductivities of partially ionized plasmas, if one uses a meanion model. Then the ion charge Z should be replaced by an effective (or average) ion charge Z_{eff}. For nondegenerate plasmas, the results are based on a continuation from the degenerate domain (using FermiDirac averaging) and can be considered as orderofmagnitude estimates. For degenerate plasmas, on the contrary, the results come from the exact theory and are expected to be much more accurate.
Potekhin A.Y., Pons J.A., Page D. Neutron Stars  Cooling and Transport, Space Sci. Rev., 191, 239 (2015)
[ArXiV:1507.06186]
The older version of the table was inaccurate for lowZ chemical elements (especially for H and He) at T around or higher than Fermi temperature, because it did not take into account electronelectron scattering.
The "long" version of the code includes the contribution of electronelectron scattering into the thermal conductivity at magnetic field B=0. However, in this case the older version still was inapplicable at T much higher than Fermi temperature, because the contribution from electronelectron scattering previously used a fit designed for strongly degenerate electrons only.
Now the highT limit of our data matches the numerical tables of Hubbard & Lampe, 1968, Astrophys. J. Suppl. 18, 297 (which remain the most accurate calculations of conductive opacities for astrophysical use in nonmagnetic, nondegenerate, weakly coupled plasma).
The ee contribution is updated in both the "long" and "short" versions of the code, as well as in the codes for the inner crust of the neutron star, according to the results by Shternin and Yakovlev [17], described above.
In early (before 2007) releases of the "long" version of the Fortran code ("conduct"), an accidental error in the ionic component of the pressure might occur (though rarely) due to a technical slip in subroutine CHEMPOT. It did not affect other data or programs presented at this site. This slip was found and eliminated on 29.04.2007.
A technical error (erroneously deleted line) has been discovered and corrected in the code "condegin" thanks to Nicolas Chamel on 12.11.2007.
Another technical slip in the "long" version of the code, some variables left uninitialized in ThAv99, which could lead (though quite rarely) to a bug, was discovered and fixed on 12.05.2011.
A new code "condBSk" is added for the inner crust of neutron stars. It is analogous to the "condegsc" code, but uses more recent nuclear form factors. Namely, the Oyamatsu (1993) approximation is now replaced by the HFB19 (BSk19), HFB20 (BSk20) and HFB21 (BSk21) models, according to the series of papers by N.Chamel, J.M.Pearson, and collaborators (20112013).
Note:This correction is available only for H and He at zero magnetic field.
The basic numerical table for interpolation is given including the "weakly damped" version of this correction. Ancillary tables without this correction, with full (nondamped) correction, and with the "strong damping" are also provided.
[make your choice and click] 

Potekhin A.Y., Pons J.A., Page D. Neutron Stars  Cooling and Transport, Space Sci. Rev., 191, 239 (2015) [arXiv:1507.06186]