On the problem of relativistic particles motion in strong magnetic field and dense matter

We consider a problem of electron motion in different media and magnetic field. It is shown that in case of nonmoving medium and constant homogenious magnetic field the electron energies are quantized. We also discuss the general problem of eigenvectors and eigenvalues of a given class of Hamiltonians. We examine obtained exact solutions for the particular case of the electron motion in a rotating neutron star with account for matter and magnetic field effects. We argue that all of these considerations can be usefull for astrophysical applications

Spin light of relativistic electrons in neutrino fluxes

AbstractA new mechanism of electromagnetic radiation by electrons under the influence of a dense neutrino flux, termed “the spin light of electron” in neutrino flux (SLeν), is considered. It is shown that in the case when electrons are moving against the neutrino flux with relativistic energy there is a reasonable increase of the efficiency of the energy transfer from the neutrino flux to the electromagnetic radiation by the SLeν mechanism. The proposed radiation process is applied to an astrophysical environment with characteristics peculiar to supernovae. It is shown that a reasonable portion of energy of the neutrino flux can be transferred by the SLeν to gamma-rays

Neutrino magnetic moment and neutrino energy quantization in rotating media

After a brief discussion on neutrino electromagnetic properties, we consider the problem of neutrino energy spectra in different media. It is shown that in two particular cases (i.e., neutrino propagation in a) transversally moving with increasing speed medium and b) rotating medium) neutrino energies are quantized. These phenomena can be important for astrophysical applications, for instance, for physics of rotating neutron stars.Comment: 7 pagex in LaTex, to appear in Proceedings of the XXIII Recontres de Physique de la Vallee D'Aoste on "Results and Perspectives in Particle Physics" (La Thuile, Italy, March 1-7, 2009

Electromagnetic field evolution in relativistic heavy-ion collisions

The hadron string dynamics (HSD) model is generalized to include the creation and evolution of retarded electromagnetic fields as well as the influence of the magnetic and electric fields on the quasiparticle propagation. The time-space structure of the fields is analyzed in detail for non-central Au+Au collisions at $\sqrt{s_{NN}}=$200 GeV. It is shown that the created magnetic field is highly inhomogeneous but in the central region of the overlapping nuclei it changes relatively weakly in the transverse direction. For the impact parameter $b=$10 fm the maximal magnetic field - perpendicularly to the reaction plane - is obtained of order $eB_y/m_\pi^2\sim$5 for a very short time $\sim$ 0.2 fm/c, which roughly corresponds to the time of a maximal overlap of the colliding nuclei. We find that at any time the location of the maximum in the $eB_y$ distribution correlates with that of the energy density of the created particles. In contrast, the electric field distribution, being also highly inhomogeneous, has a minimum in the center of the overlap region. Furthermore, the field characteristics are presented as a function of the collision energy and the centrality of the collisions. To explore the effect of the back reaction of the fields on hadronic observables a comparison of HSD results with and without fields is exemplified. Our actual calculations show no noticeable influence of the electromagnetic fields - created in heavy-ion collisions - on the effect of the electric charge separation with respect to the reaction plane.Comment: 17 pages, 22 figures, title changed by editor, accepted for PR

Neutrino photoproduction on the electron in dense magnetized medium

The process of neutrino photoproduction on an electron, e γ   →   e v v ¯ , in a strongly magnetized cold plasma in resonant case has been considered. The contribution of this process to the neutrino emissivity has been calculated. It has been shown that under such conditions neutrino emissivity due to process e γ   →   e v v ¯ could be expressed in terms of emissivity of it's subprocess, e   →   e v v ¯