arXiv subjects

A. Kandus

Publications and source records attributed to A. Kandus.

3 recordsLinked to original sources

arXiv2006

On the mean field dynamo with Hall effect

We study in the present paper how Hall effect modifies the quenching process of the electromotive force (e.m.f.) in Mean Field Dynamo (MFD) theories. We write down the evolution equations for the e.m.f. and for the large and small scale magnetic helicity, treat Hall effect as a perturbation and integrate the resulting equations assuming boundary conditions such that the total divergencies vanish. For force-free large scale magnetic fields, Hall effect acts by coupling the small scale velocity and magnetic fields. For the range of parameters considered, the overall effect is a stronger quenching of the e.m.f. than in standard MHD and a damping of the inverse cascade of magnetic helicity. In astrophysical environments characterized by the parameters considered here, Hall effect would produce an earlier quenching of the e.m.f. and consequently a weaker large scale magnetic field.

astro-ph↗

arXiv2004

Origin of coherent magnetic fields in high redshift objects

Large scale strong magnetic fields in galaxies are generally thought to have been generated by a mean field dynamo. In order to have generated the fields observed, the dynamo would have had to have operated for a sufficiently long period of time. However, magnetic fields of similar intensities and scales to the one in our galaxy, are observed in high redshift galaxies, where a mean field dynamo would not have had enough time to produce the observed fields. Instead of a mean field dynamo, we study the emergence of strong large scale magnetic fields in the first objects formed in the universe due to the action or a turbulent, helical stochastic dynamo, for redshifts $5 \leq z \leq 10$. Ambipolar drift plays an important role in this process due to the low level of ionization of the gas, allowing a large scale stochastic dynamo to operate. We take into account the uncertainties in the physics of high redshift objects by examining a range of values for the parameters that characterize the turbulent plasma. By numerically integrating the nonlinear evolution equations for the magnetic field correlations, we show that for reasonable values of the parameters in the time interval considered, fields can grow to high intensities ($\sim 10^{-6}$ G), with large coherence lengths ($\sim 2-6$ kpc), essentially independent of the initial values of the magnetic field.

astro-ph↗

arXiv2003

Dependence of the MHD shock thickness on the finite electrical conductivity

The results of MHD plane shock waves with infinite electrical conductivity are generalized for a plasma with a finite conductivity. We derive the adiabatic curves that describe the evolution of the shocked gas as well as the change in the entropy density. For a parallel shock (i.e., in which the magnetic field is parallel to the normal to the shock front) we find an expression for the shock thickness which is a function of the ambient magnetic field and of the finite electrical conductivity of the plasma. We give numerical estimates of the physical parameters for which the shock thickness is of the order of, or greater than, the mean free path of the plasma particles in a strongly magnetized plasma.

physics.plasm-ph↗