arXiv subjects

A. D. Kaminker

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

40 records · Page 3Linked to original sources

arXiv1997

Neutrino synchrotron emission from dense magnetized electron gas of neutron stars

We study the synchrotron emission of neutrino pairs by relativistic, degenerate electrons in strong magnetic fields. Particular attention is paid to the case in which the dominant contribution comes from one or several lowest cyclotron harmonics. Calculations are performed using the exact quantum formalism and the quasiclassical approach. Simple analytic fits to the neutrino synchrotron emissivity are obtained in the domain of magnetized, degenerate and relativistic electron gas provided the electrons populate either many Landau levels or the ground level alone. The significance of the neutrino synchrotron energy losses in the interiors of cooling neutron stars is discussed.

astro-ph↗

arXiv1997

Neutrino pair emission due to scattering of electrons off fluxoids in superfluid neutron star cores

We study the emission of neutrinos, resulting from the scattering of electrons off magnetic flux tubes (fluxoids) in the neutron star cores with superfluid (superconducting) protons. In the absence of proton superfluidity (T> T_{cp}), this process transforms into the well known electron synchrotron emission of neutrino pairs in a locally uniform magnetic field B, with the neutrino energy loss rate Q proportional to B^2 T^5. For temperatures T not much below T_{cp}, the synchrotron regime (Q \propto T^5) persists and the emissivity Q can be amplified by several orders of magnitude due to the appearance of the fluxoids and associated enhancement of the field within them. For lower T, the synchrotron regime transforms into the bremsstrahlung regime (Q \propto T^6) similar to the ordinary neutrino-pair bremsstrahlung of electrons which scatter off atomic nuclei. We calculate Q numerically and represent our results through a suitable analytic fit. In addition, we estimate the emissivities of two other neutrino-production mechanisms which are usually neglected -- neutrino-pair bremsstrahlung processes due to electron-proton and electron-electron collisions. We show that the electron-fluxoid and electron-electron scattering can provide the main neutrino production mechanisms in the neutron star cores with highly superfluid protons and neutrons at T < 5 10^8 K. The electron-fluxoid scattering is significant if the initial, locally uniform magnetic field B > 10^{13} G.

astro-ph↗

arXiv1996

Neutrino-Pair Emission due to Electron-Phonon Scattering in a Neutron Star Crust

Neutrino-pair bremsstrahlung radiation is considered due to electron--phonon scattering of degenerate, relativistic electrons in a lattice of spherical atomic nuclei in a neutron star crust. The neutrino energy generation rate is calculated taking into account exact spectrum of phonons, the Debye--Waller factor, and the nuclear form--factor in the density range from $10^7$~g~cm$^{-3}$ to $10^{14}$~g~cm$^{-3}$ at arbitrary nuclear composition for body-centered-cubic and face-centered-cubic Coulomb crystals. The results are fitted by a unified analytic expression. A comparison is given of the neutrino bremsstrahlung energy losses in a neutron star crust composed of ground state and accreted matter, in the solid and liquid phases.

astro-ph↗

arXiv1996

Electron $ν\barν$ Bremsstrahlung in a Liquid Phase of Neutron Star Crusts

Neutrino emissivity from the electron $ν\barν$ bremsstrahlung in the liquid layers of the neutron star crusts is studied. Nuclear composition of matter in neutron star crusts is considered for various scenarios of neutron star evolution. For the deep layers of the crust, the compositions of cold catalyzed matter, accreted matter and hot matter ($T \ga 5 \times 10^9$~K) are shown to be very different, and this implies differences in the neutrino emissivity at given density and temperature. Neutrino-pair bremsstrahlung, due to collisions of relativistic degenerate electrons in a Coulomb liquid of atomic nuclei, is considered. The neutrino energy loss rate is expressed in a simple form through a Coulomb logarithm $L$ -- a slowly varying function of density, temperature, and nuclear composition. Non-Born corrections, thermal width of electron Fermi sphere, and finite sizes of nuclei are taken into account. Implications for cooling of neutron stars are discussed.

astro-ph↗