Pushkov Institute of Terrestrial Magnetism

Saint Petersburg, Russia

Pushkov Institute of Terrestrial Magnetism

Saint Petersburg, Russia
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Dvornikov M.,University of Sao Paulo | Dvornikov M.,Pushkov Institute of Terrestrial Magnetism
Journal of Atmospheric and Solar-Terrestrial Physics | Year: 2013

We study nano-sized spherically symmetric plasma structures which are radial nonlinear oscillations of electrons in plasma. The effective interaction of these plasmoids via quantum exchange forces between ions is described. We calculate the energy of this interaction for the case of a dense plasma. The conditions when the exchange interaction is attractive are examined and it is shown that separate plasmoids can form a single object. The application of our results to the theoretical description of stable atmospheric plasma structures is considered. © 2012 Elsevier Ltd.


Dvornikov M.,University of Sao Paulo | Dvornikov M.,Pushkov Institute of Terrestrial Magnetism
Foundations of Physics | Year: 2012

We construct a consistent theory of a quantum massive Weyl field. We start with the formulation of the classical field theory approach for the description of massive Weyl fields. It is demonstrated that the standard Lagrange formalism cannot be applied for the studies of massive first-quantized Weyl spinors. Nevertheless we show that the classical field theory description of massive Weyl fields can be implemented in frames of the Hamilton formalism or using the extended Lagrange formalism. Then we carry out a canonical quantization of the system. The independent ways for the quantization of a massive Weyl field are discussed. We also compare our results with the previous approaches for the treatment of massive Weyl spinors. Finally the new interpretation of the Majorana condition is proposed. © 2012 Springer Science+Business Media, LLC.


Dvornikov M.,University of Sao Paulo | Semikoz V.B.,Pushkov Institute of Terrestrial Magnetism
Physical Review D - Particles, Fields, Gravitation and Cosmology | Year: 2013

We study lepton asymmetry evolution in plasma of the early Universe before the electroweak phase transition (EWPT) accounting for chirality flip processes via Higgs decays (inverse decays) entering equilibrium at temperatures below TRL≠10 TeV, TEW


Dvornikov M.,University of Sao Paulo | Dvornikov M.,Tomsk State University | Semikoz V.B.,Pushkov Institute of Terrestrial Magnetism
Physical Review D - Particles, Fields, Gravitation and Cosmology | Year: 2015

We show that the Standard Model electroweak interaction of ultrarelativistic electrons with nucleons (the eN interaction) in a neutron star (NS) permeated by a seed large-scale helical magnetic field provides its growth up to 1015G during a time comparable with the ages of young magnetars ∼104yr. The magnetic field instability originates from the parity violation in the eN interaction entering the generalized Dirac equation for right and left massless electrons in an external uniform magnetic field. We calculate the average electric current given by the solution of the modified Dirac equation containing an extra current for right and left electrons (positrons), which turns out to be directed along the magnetic field. Such a current includes both a changing chiral imbalance of electrons and the eN potential given by a constant neutron density in a NS. Then we derive the system of the kinetic equations for the chiral imbalance and the magnetic helicity which accounts for the eN interaction. By solving this system, we show that a sizable chiral imbalance arising in a neutron protostar due to the Urca process eL-+p→N+νeL diminishes very rapidly because of a huge chirality-flip rate. Thus the eN term prevails over the chiral effect, providing a huge growth of the magnetic helicity and the helical magnetic field. © 2015 American Physical Society.


Dvornikov M.,University of Sao Paulo | Dvornikov M.,Tomsk State University | Semikoz V.B.,Pushkov Institute of Terrestrial Magnetism
Journal of Cosmology and Astroparticle Physics | Year: 2015

We study the instability of magnetic fields in a neutron star core driven by the parity violating part of the electron-nucleon interaction in the Standard Model. Assuming a seed field of the order 1012 G, that is a common value for pulsars, one obtains its amplification due to such a novel mechanism by about five orders of magnitude, up to 1017 G, at time scales ∼ (103-105) yr. This effect is suggested to be a possible explanation of the origin of the strongest magnetic fields observed in magnetars. The growth of a seed magnetic field energy density is stipulated by the corresponding growth of the magnetic helicity density due to the presence of the anomalous electric current in the Maxwell equation. Such an anomaly is the sum of the two competitive effects: (i) the chiral magnetic effect driven by the difference of chemical potentials for the right and left handed massless electrons and (ii) constant chiral electroweak electron-nucleon interaction term, which has the polarization origin and depends on the constant neutron density in a neutron star core. The remarkable issue for the decisive role of the magnetic helicity evolution in the suggested mechanism is the arbitrariness of an initial magnetic helicity including the case of non-helical fields from the beginning. The tendency of the magnetic helicity density to the maximal helicity case at large evolution times provides the growth of a seed magnetic field to the strongest magnetic fields in astrophysics. © 2015 IOP Publishing Ltd and Sissa Medialab srl .


Dvornikov M.,University of Sao Paulo | Dvornikov M.,Pushkov Institute of Terrestrial Magnetism
Journal of Cosmology and Astroparticle Physics | Year: 2013

We derive the new quasi-classical equation for the description of the spin evolution of a neutrino propagating in a curved space-time and interacting with a background matter and an external electromagnetic field. This equation is used to analyze neutrino spin oscillations in these external backgrounds. We obtain the effective Hamiltonian and the transition probability for oscillations of neutrinos when they move in the vicinity of a rotating black hole, surrounded by an accretion disk, and interact with an external magnetic field. The appearance of new resonances in neutrino spin oscillations in this system is considered. The approximate treatment of spin oscillations of radially propagating ultra high energy neutrinos is developed. We also discuss the applications of our results to the description of neutrino spin oscillations in realistic astrophysical media. © 2013 IOP Publishing Ltd and Sissa Medialab srl.


Dvornikov M.,University of Sao Paulo | Dvornikov M.,Pushkov Institute of Terrestrial Magnetism
Journal of Physics A: Mathematical and Theoretical | Year: 2013

We study a quantum spherically symmetric object which is based on radial plasma oscillations. Such a plasmoid is supposed to exist in a dense plasma containing electrons, ions and neutral particles. The method of creation and annihilation operators is applied to quantize the motion of charged particles in a self-consistent potential. We also study the effective interaction between oscillating particles owing to the exchange of a virtual acoustic wave, which is excited in the neutral component of plasma. It is shown that this interaction can be attractive and result in the formation of ion pairs. We discuss possible applications of this phenomenon in astrophysical and terrestrial plasmas. © 2013 IOP Publishing Ltd.


Zirakashvili V.N.,Pushkov Institute of Terrestrial Magnetism | Ptuskin V.S.,Pushkov Institute of Terrestrial Magnetism
Astroparticle Physics | Year: 2016

It is shown that high-energy astrophysical neutrinos observed in the IceCube experiment can be produced by protons accelerated in extragalactic Type IIn supernova remnants by shocks propagating in the dense circumstellar medium. The nonlinear diffusive shock acceleration model is used for description of particle acceleration. We calculate the neutrino spectrum produced by an individual Type IIn supernova and the spectrum of neutrino background produced by IIn supernovae in the expanding Universe. We also found that the arrival direction of one Icecube neutrino candidate (track event 47) is at 1.35° from Type IIn supernova 2005bx. © 2016 Elsevier B.V. All rights reserved.


Sidorova L.N.,Pushkov Institute of Terrestrial Magnetism | Filippov S.V.,Pushkov Institute of Terrestrial Magnetism
Journal of Atmospheric and Solar-Terrestrial Physics | Year: 2012

The idea of an equatorial origin of the He + density depletions (HDDs) was validated once again. For this purpose, detailed comparative analysis of their longitudinal occurrence distributions (for all seasons and different hemispheres) was made. The distributions during the equinox periods were found to be very similar to the distributions of the equatorial F-region irregularities (EFIs), equatorial spread F (EFS) and equatorial plasma bubbles (EPBs). However, the similarity was not so good for the solstice periods due to complex influence of the seasonal factor, "magnetic declination effect" and thermospheric meridional winds. The results obtained may be considered as new evidence supporting the idea of the plasma bubble origin of the HDDs. © 2012 Elsevier Ltd.


This paper investigates the relationship between cyclic variations in the velocity of coronal mass ejections and cyclic changes in the structure of the large-scale solar magnetic field (LSSMF) in solar cycle 23, using the effective solar multipole index as a parameter of the characteristic dimensions of LSSMF structural elements. Cyclic variations in the velocity and frequency of coronal mass ejections are found to resemble cyclic changes in the effective solar multipole index. It is suggested that cyclic changes in the maximum velocity of coronal mass ejections are associated with different conditions for the formation of complexes of active regions connected by coronal arch structures, the energy of which is the main source of energy (velocity) for coronal mass ejections. The study leads to some suggestions about the possible site of initiation of coronal mass ejections. © 2012 Pleiades Publishing, Ltd.

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