13 research outputs found
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 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 10 fm the maximal magnetic field - perpendicularly to the
reaction plane - is obtained of order 5 for a very short time
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 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
¯