3,848 research outputs found
On temperature-dependent anisotropies of upper critical field and London penetration depth
We show on a few examples of one-band materials with spheroidal Fermi
surfaces and anisotropic order parameters that anisotropies of the
upper critical field and of the London penetration depth
depend on temperature, the feature commonly attributed to multi-band
superconductors. The parameters and may have
opposite temperature dependencies or may change in the same direction depending
on Fermi surface shape and on character of the gap nodes. For two-band systems,
the behavior of anisotropies is affected by the ratios of bands densities of
states, Fermi velocities, anisotropies, and order parameters. We investigate in
detail the conditions determining the directions of temperature dependences of
the two anisotropy factors
Two-Stream Instability of Counter-Rotating Galaxies
The present study of the two-stream instability in stellar disks with
counter-rotating components of stars and/or gas is stimulated by recently
discovered counter-rotating spiral and S0 galaxies. Strong linear two-stream
instability of tightly-wrapped spiral waves is found for one and two-armed
waves with the pattern angular speed of the unstable waves always intermediate
between the angular speed of the co-rotating matter () and that of the
counter-rotating matter (). The instability arises from the
interaction of positive and negative energy modes in the co- and
counter-rotating components. The unstable waves are in general convective -
they move in radius and radial wavenumber space - with the result that
amplification of the advected wave is more important than the local growth
rate. For a galaxy of co-rotating stars and counter-rotating stars of
mass-fraction , or of counter-rotating gas of mass-fraction
, the largest amplification is usually for the one-armed
leading waves (with respect to the co-rotating stars). For the case of both
counter-rotating stars and gas, the largest amplifications are for , also for one-armed leading waves. The two-armed trailing
waves usually have smaller amplifications. The growth rates and amplifications
all decrease as the velocity spreads of the stars and/or gas increase. It is
suggested that the spiral waves can provide an effective viscosity for the gas
causing its accretion.Comment: 14 pages, submitted to ApJ. One table and 17 figures can be obtained
by sending address to R. Lovelace at [email protected]
Accretion into black holes with magnetic fields, and relativistic jets
We discuss the problem of the formation of a large-scale magnetic field in
the accretion disks around black holes, taking into account the non-uniform
vertical structure of the disk. The high electrical conductivity of the outer
layers of the disk prevents the outward diffusion of the magnetic field. This
implies a stationary state with a strong magnetic field in the inner parts of
the accretion disk close to the black hole, and zero radial velocity at the
surface of the disk. Structure of advective accretion disks is investigated,
and conditions for formation of optically thin regions in central parts of the
accretion disk are found. The problem of jet collimation by magneto-torsion
oscillations is considered.Comment: 6 pages, 4 figure
Current fluctuations near to the 2D superconductor-insulator quantum critical point
Systems near to quantum critical points show universal scaling in their
response functions. We consider whether this scaling is reflected in their
fluctuations; namely in current-noise. Naive scaling predicts low-temperature
Johnson noise crossing over to noise power at strong
electric fields. We study this crossover in the metallic state at the 2d z=1
superconductor/insulator quantum critical point. Using a Boltzmann-Langevin
approach within a 1/N-expansion, we show that the current noise obeys a scaling
form with . We recover
Johnson noise in thermal equilibrium and at strong
electric fields. The suppression from free carrier shot noise is due to strong
correlations at the critical point. We discuss its interpretation in terms of a
diverging carrier charge or as out-of-equilibrium Johnson
noise with effective temperature .Comment: 5 page
Vertical Structure of Stationary Accretion Disks with a Large-Scale Magnetic Field
In earlier works we pointed out that the disk's surface layers are
non-turbulent and thus highly conducting (or non-diffusive) because the
hydrodynamic and/or magnetorotational (MRI) instabilities are suppressed high
in the disk where the magnetic and radiation pressures are larger than the
plasma thermal pressure. Here, we calculate the vertical profiles of the {\it
stationary} accretion flows (with radial and azimuthal components), and the
profiles of the large-scale, magnetic field taking into account the turbulent
viscosity and diffusivity and the fact that the turbulence vanishes at the
surface of the disk.
Also, here we require that the radial accretion speed be zero at the disk's
surface and we assume that the ratio of the turbulent viscosity to the
turbulent magnetic diffusivity is of order unity. Thus at the disk's surface
there are three boundary conditions. As a result, for a fixed dimensionless
viscosity -value, we find that there is a definite relation between the
ratio of the accretion power going into magnetic disk winds to the
viscous power dissipation and the midplane plasma-, which is the ratio
of the plasma to magnetic pressure in the disk. For a specific disk model with
of order unity we find that the critical value required for a
stationary solution is , where the disk's
half thickness. For weaker magnetic fields, , we argue that
the poloidal field will advect outward while for it will
advect inward. Alternatively, if the disk wind is negligible (), there are stationary solutions with .Comment: 5 pages, 3 figure
Interquark Potential in Schrodinger Representation
Static charges are introduced in Yang-Mills theory via coupling to heavy
fermions. The states containing static color charges are constructed using
integration over gauge transformations. A functional representation for
interquark potential is obtained. This representation provides a simple
criterion for confinement.Comment: 9pp., Late
Large Scale B-Field in Stationary Accretion Disks
We reconsider the problem of the formation of a large-scale magnetic field in
the accretion disks around black holes. In contrast with previous work we take
into account the nonuniform vertical structure of the disk. The high electrical
conductivity of the outer layers of the disk prevents the outward diffusion of
the magnetic field. This implies a stationary state with a strong magnetic
field in the inner parts of the accretion disk close to the black hole.Comment: 5 pages, 2 figure
Comptonization signatures in the rapid aperiodic variability of Galactic black-hole candidates
We investigate the effect of inverse-Compton scattering of flares of soft
radiation in different geometries of a hot, Comptonizing region and a colder
accretion disk around a solar-mass black hole. The photon-energy dependent
light curves, their Fourier transforms, power spectra and Fourier-period
dependent time lags of hard photons with respect to softer photons are
discussed. On the basis of a comparison with existing data we find arguments
against Comptonization of external soft radiation as well as Comptonization in
a homogeneous medium as dominant mechanisms for the rapid aperiodic variability
in Galactic black-hole candidates. Possible further observational tests for the
influence of Comptonization on the rapid aperiodic variability of Galactic
black-hole candidates are suggested.Comment: 32 pages, including 10 figures and 2 tables; uses epsf.sty,
rotate.sty; submitted to Ap
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