Magnetic reconnection can be interpreted as a process in which the electromagnetic eld is frozen into a four-velocity eld in Minkowski space. For reconnec-tion to occur the four-velocity eld has to be a special type of stagnation ow. Prescribing this type of ow in a nite spatial domain allows the modelling of localized reconnection events and the investigation of examples of reconnection in reg...

We consider the hypothesis that galactic magnetic elds are primordial. We also discuss the various objections to this hypothesis. We assume that there was a magnetic eld present in the galactic plasma before the galaxy formed. After the galactic disk formed, the lines of force thread through it and remain connected to the external cosmic medium. They enter through one side of the disk, proceed ...

This study presents cross-sectional vector maps of the magnetic ®eld derived from IMP 8 magnetometer in the magnetosheath at 30 Re behind the Earth. In addition the vector patterns of the magnetosheath ®eld for northward, southward, and east-west interplanetary magnetic ®eld (IMF) directions are qualitatively compared with those obtained from the Spreiter-Stahara gas dynamic (GD) and Fedder-Lyo...

In this paper, by considering a simple uid model, we investigate the role of phase transitions in the ISM on the galaxy scale gas dynamics. Cooling and heating timescales in the ISM are typically shorter than typical galactic rotation timescales, so the individual phases in the ISM can be assumed to be in temperature equilibrium with the radiation eld. Using this approximation we can construct ...

This essay investigates the magnetoviscous properties of ferro uid ow in both an external magnetic eld and in zero eld. Zeroeld properties of ferro uids are examined. Phenomena such as the dramatic increase in ferro uid viscosity in the presensce of a static eld as well as negative viscosity for an alternating magnetic eld are described.

The evolution of supernova remnants (SNRs) is studied, with particular attention to the effect of magnetic fields with axisymmetric two-dimensional magnetohydrodynamical simulations. The evolution of magnetic SNRs is the same as non-magnetic ones in the adiabatic Sedov stage. After a thin shell is formed, the shell is driven by the pressure of the hot interior gas (bubble). Evolution in the pre...

Magnetic levitation experiments have been performed on arabidopsis plants equipped with a stress responsive reporter gene system Seedlings were levitated in a magnetic eld gradient B T and BrB T m for hours and control specimens were located at the center of the magnet B T and in a low eld B mT region The reporter gene qualitatively indicates that the levitated and the magnetic eld control spec...

Magnetic eld is present in most of the chemically peculiar stars of the upper main sequence. For a long time, the component of the magnetic eld along the line of sight and the magnetic eld modulus, averaged on the stellar disk, were the only diagnostic contents of the observational techniques. Recent developments in the application of the theory of line formation, joined to the increased sensit...

The dynamical effects of magnetic fields in models of radiative, Herbig-Haro (HH) jets have been studied in a number of papers. For example, magnetized, radiative jets from variable sources have been studied with axisymmetric and 3D numerical simulations. In this paper, we present an analytic model describing the effect of a toroidal magnetic field on the internal working surfaces that result f...