arXiv subjects

D. A. Baiko

Publications and source records attributed to D. A. Baiko.

28 records · Page 2Linked to original sources

arXiv2001

Thermodynamic functions of harmonic Coulomb crystals

Phonon frequency moments and thermodynamic functions (electrostatic and vibrational parts of the free energy, internal energy, and heat capacity) are calculated for bcc and fcc Coulomb crystals in the harmonic approximation with a fractional accuracy within one part on 10^5. Temperature dependence of thermodynamic functions is fitted by analytic formulas with an accuracy of a few parts in 10^5. The static-lattice (Madelung) part of the free energy is calculated with an accuracy about 10^{-12}. The Madelung constant and frequency moments of hcp crystals are also computed.

physics.plasm-ph↗

arXiv2001

Thermal Conductivity of Neutrons in Neutron Star Cores

The diffusive thermal conductivity of neutrons in dense matter [$ρ\sim (1 - 8) \times 10^{14}$ g cm$^{-3}$] of neutron star cores is calculated. The contribution from neutron--neutron and neutron--proton collisions is taken into account. We use the transition probabilities calculated for symmetric dense nucleon matter on the basis of the Dirac--Brueckner approach to the in-medium effects and the Bonn model of bare nucleon--nucleon interaction. The diffusive thermal conductivity of neutrons in the presence of neutron and proton superfluidities is analyzed in a microscopic manner; the effects of superfluidity are shown to be significant. The low temperature behavior of the thermal conductivity appears to be extremely sensitive to the relation between critical temperatures of neutrons and protons. The results are fitted by simple analytic expressions. In combination with the formulae for the electron and muon thermal conductivities, obtained earlier, the present expressions provide a realistic description of the full diffusive thermal conductivity in the neutron star cores for normal and various superfluid phases.

astro-ph↗

arXiv2000

Cooling neutron stars with localized protons

We analyze cooling of neutron stars, assuming the presence of localized protons in the densest region of their cores. Choosing a single threshold density for proton localization and adjusting neutron star mass, we reproduce the observational data on effective surface temperatures of Vela and PSR 0656+14, with or without an accreted hydrogen envelope. However, the presence of a tiny hydrogen envelope is mandatory, in this model, for reproducing the Geminga data.

astro-ph↗

arXiv1999

Coulomb crystals in the harmonic lattice approximation

The dynamic structure factor ${\tilde S}({\bf k},ω)$ and the two-particle distribution function $g({\bf r},t)$ of ions in a Coulomb crystal are obtained in a closed analytic form using the harmonic lattice (HL) approximation which takes into account all processes of multi-phonon excitation and absorption. The static radial two-particle distribution function $g(r)$ is calculated for classical ($T \gtrsim \hbar ω_p$, where $ω_p$ is the ion plasma frequency) and quantum ($T \ll \hbar ω_p$) body-centered cubic (bcc) crystals. The results for the classical crystal are in a very good agreement with extensive Monte Carlo (MC) calculations at $1.5 \lesssim r/a \lesssim 7$, where $a$ is the ion-sphere radius. The HL Coulomb energy is calculated for classical and quantum bcc and face-centered cubic crystals, and anharmonic corrections are discussed. The inelastic part of the HL static structure factor $S''(k)$, averaged over orientations of wave-vector {\bf k}, is shown to contain pronounced singularities at Bragg diffraction positions. The type of the singularities is different in classical and quantum cases. The HL method can serve as a useful tool complementary to MC and other numerical methods.

physics.plasm-ph↗

arXiv1999

Transport properties and neutrino emissivity of dense neutron-star matter with localized protons

As pointed out by Kutschera and W{ó}jcik, very low concentration of protons combined with a specific density dependence of effective neutron-proton interaction could lead to a localization of ``proton impurities'' in neutron medium at densities exceeding four times normal nuclear matter density. We study consequences of the localization of protons for transport processes in dense neutron star cores, assuming random distribution of proton impurities. Kinetic equations, relevant for the transport of charge, heat and momentum, are solved using variational method. Localization of protons removes a T^{-2} factor from the transport coefficients, which leads, at lower temperatures, to a strong decrease of thermal conductivity, electrical conductivity and shear viscosity of neutron star matter, as compared to the standard case, where protons form a Fermi liquid. Due to the localization of protons a number of conventional neutrino emission processes (including modified URCA process) become inoperative in neutron star cores. On the other hand, the energy loss rate from neutrino-antineutrino pair bremsstrahlung due to electron and neutron scattering off (localized) protons, will have a specific T^6 dependence, which could modify the cooling of the neutron star core, as compared to the standard case. Possible astrophysical implications of the localization of protons for neutron star evolution and dynamics are discussed.

astro-ph↗

arXiv1999

Transport properties of degenerate electrons in neutron star envelopes and white dwarf cores

New calculations of the thermal and electrical electron conductivities are performed for a broad range of physical parameters typical for envelopes of neutron stars and cores of white dwarfs. We consider stellar matter composed of astrophysically important chemical elements from H to Fe in the density range from 10^2-10^4 g/ccm up to 10^7-10^{10} g/ccm, where atoms are fully ionized and electrons are strongly degenerate. We have used modified ion structure factors suggested in physics/9811052. In the ion liquid, these modifications take into account, in an approximate way, instantaneous electron-band structures that reduce the electron-ion scattering rate. In crystallized matter, the new structure factors include multi-phonon processes important at temperatures not very much lower than the melting temperature T_m. The transport coefficients obtained differ significantly from those derived earlier in the important temperature range T_m/5 < T < 5 T_m. The results of our numerical calculations are fitted by analytical expressions convenient for astrophysical applications.

astro-ph↗

arXiv1998

Direct Urca process in strong magnetic fields and neutron star cooling

The effect of the magnetic field on the energy loss rate in the direct Urca reactions is studied. The general expression for the neutrino emissivity at arbitrary magnetic field B is derived. The main emphasis is laid on a case, in which the field is not superstrong, and charged reacting particles (e and p) populate many Landau levels. The magnetic field keeps the process operative if Delta k / k_{Fn} < N_{Fp}^{-2/3} (N_{Fp} is the number of the Landau levels populated by protons and Delta k = k_{Fn}-k_{Fp}-k_{Fe}), that is beyond the well-known switch-on limit in the absence of the field, Delta k < 0. Cooling of magnetized neutron stars with strong neutron superfluid in the outer cores and nonsuperfluid inner cores is simulated. The magnetic field near the stellar center speeds up the cooling if the stellar mass M is slightly less than the minimum mass M_c at which the direct Urca reaction becomes allowed for B=0. If B=3x10^{16} G the affected mass range is M_c-M < 0.1M_c, while for B=3x10^{15} G the range is M_c-M < 0.015M_c. This may influence a theoretical interpretation of the observed thermal radiation as illustrated for the Geminga pulsar. The case of superstrong magnetic fields (B>10^{18} G), such that e and p populate only the lowest Landau levels is briefly outlined.

astro-ph↗

arXiv1998

Ion structure factors and electron transport in dense Coulomb plasmas

The dynamical structure factor of a Coulomb crystal of ions is calculated at arbitrary temperature below the melting point taking into account multi-phonon processes in the harmonic approximation. In a strongly coupled Coulomb ion liquid, the static structure factor is split into two parts, a Bragg-diffraction-like one, describing incipient long-range order structures, and an inelastic part corresponding to thermal ion density fluctuations. It is assumed that the diffractionlike scattering does not lead to the electron relaxation in the liquid phase. This assumption, together with the inclusion of multi-phonon processes in the crystalline phase, eliminates large discontinuities of the transport coefficients (jumps of the thermal and electric conductivities, as well as shear viscosity, reported previously) at a melting point.

physics.plasm-ph↗

arXiv1996

Thermal and Electric Conductivities of Coulomb Crystals in Neutron Stars and White Dwarfs

Thermal and electric conductivities are calculated for degenerate electrons scattered by phonons in a crystal made of atomic nuclei. The exact phonon spectrum and the Debye--Waller factor are taken into account. Monte Carlo calculations are performed for body-centered cubic (bcc) crystals made of C, O, Ne, Mg, Si, S, Ca, and Fe nuclei in the density range from $10^3$ to $10^{11}$ g cm$^{-3}$ at temperatures lower than the melting temperature but higher than the temperature at which the Umklapp processes begin to be "frozen out". A simplified method of calculation is proposed, which makes it possible to describe the results in terms of simple analytic expressions, to extend these expressions to any species of nucleus, and to consider face-centered cubic (fcc) crystals. The kinetic coefficients are shown to depend tangibly on the lattice type. The results are applicable to studies of heat transfer and evolution of the magnetic field in the cores of white dwarfs and in the crusts of neutron stars. The thermal drift of the magnetic field in the crust of a neutron star is discussed.

astro-ph↗

arXiv1996

Thermal and Electric Conductivities of Coulomb Crystals in the Inner Crust of a Neutron Star

Thermal and electric conductivities of relativistic degenerate electrons are calculated for the case when electrons scatter by phonons in Coulomb crystals made of spherical finite--size nuclei at densities $10^{11}$~g/cm$^3 < ρ< 10^{14}$~g/cm$^3$, corresponding to the inner crust of a neutron star. In combination with the results of the previous article (for lower $ρ$), simple unified fits are obtained which describe the kinetic coefficients in the range $10^3$~g/cm$^3 < ρ< 10^{14}$~g/cm$^3$, for matter with arbitrary nuclear composition. The results are valid for studying thermal evolution of neutron stars and evolution of their magnetic fields. The difference between the kinetic coefficients in the neutron star crust composed of ground state and accreted matters is analyzed. Thermal drift of the magnetic field in the neutron star crust is discussed.

astro-ph↗