211 research outputs found
Kink instabilities in jets from rotating magnetic fields
We have performed 2.5D and 3D simulations of conical jets driven by the
rotation of an ordered, large-scale magnetic field in a stratified atmosphere.
The simulations cover about three orders of magnitude in distance to capture
the centrifugal acceleration as well as the evolution past the Alfven surface.
We find that the jets develop kink instabilities, the characteristics of which
depend on the velocity profile imposed at the base of the flow. The
instabilities are especially pronounced with a rigid rotation profile, which
induces a shearless magnetic field. The jet's expansion appears to be limiting
the growth of Alfven mode instabilities.Comment: 10 pages, 13 figures, accepted for publication in A&
STM imaging of electronic waves on the surface of BiTe: topologically protected surface states and hexagonal warping effects
Scanning tunneling spectroscopy studies on high-quality BiTe crystals
exhibit perfect correspondence to ARPES data, hence enabling identification of
different regimes measured in the local density of states (LDOS). Oscillations
of LDOS near a step are analyzed. Within the main part of the surface band
oscillations are strongly damped, supporting the hypothesis of topological
protection. At higher energies, as the surface band becomes concave,
oscillations appear which disperse with a particular wave-vector that may
result from an unconventional hexagonal warping term.Comment: 4 pages, 4 figures. Revised manuscript with improved analysis and
figure
Cosine and Sine Operators Related with Orthogonal Polynomial Sets on the Intervall [-1,1]
The quantization of phase is still an open problem. In the approach of
Susskind and Glogower so called cosine and sine operators play a fundamental
role. Their eigenstates in the Fock representation are related with the
Chebyshev polynomials of the second kind. Here we introduce more general cosine
and sine operators whose eigenfunctions in the Fock basis are related in a
similar way with arbitrary orthogonal polynomial sets on the intervall [-1,1].
To each polynomial set defined in terms of a weight function there corresponds
a pair of cosine and sine operators. Depending on the symmetry of the weight
function we distinguish generalized or extended operators. Their eigenstates
are used to define cosine and sine representations and probability
distributions. We consider also the inverse arccosine and arcsine operators and
use their eigenstates to define cosine-phase and sine-phase distributions,
respectively. Specific, numerical and graphical results are given for the
classical orthogonal polynomials and for particular Fock and coherent states.Comment: 1 tex-file (24 pages), 11 figure
3D Relativistic Magnetohydrodynamic Simulations of Magnetized Spine-Sheath Relativistic Jets
Numerical simulations of weakly magnetized and strongly magnetized
relativistic jets embedded in a weakly magnetized and strongly magnetized
stationary or weakly relativistic (v = c/2) sheath have been performed. A
magnetic field parallel to the flow is used in these simulations performed by
the new GRMHD numerical code RAISHIN used in its RMHD configuration. In the
numerical simulations the Lorentz factor jet is precessed to
break the initial equilibrium configuration. In the simulations sound speeds
are in the weakly magnetized simulations and in the strongly magnetized simulations. The Alfven wave speed is
in the weakly magnetized simulations and in
the strongly magnetized simulations. The results of the numerical simulations
are compared to theoretical predictions from a normal mode analysis of the
linearized relativistic magnetohydrodynamic (RMHD) equations capable of
describing a uniform axially magnetized cylindrical relativistic jet embedded
in a uniform axially magnetized relativistically moving sheath. The theoretical
dispersion relation allows investigation of effects associated with maximum
possible sound speeds, Alfven wave speeds near light speed and relativistic
sheath speeds. The prediction of increased stability of the weakly magnetized
system resulting from c/2 sheath speeds and the stabilization of the strongly
magnetized system resulting from c/2 sheath speeds is verified by the numerical
simulation results.Comment: 31 pages, 8 figures, accepted for publicatin in ApJ. A paper with
high resolution figures available at
http://gammaray.nsstc.nasa.gov/~mizuno/research_new.htm
Three-Dimensional Simulations of Inflows Irradiated by a Precessing Accretion Disk in Active Galactic Nuclei: Formation of Outflows
We present three-dimensional (3-D) hydrodynamical simulations of gas flows in
the vicinity of an active galactic nucleus (AGN) powered by a precessing
accretion disk. We consider the effects of the radiation force from such a disk
on its environment on a relatively large scale (up to ~10 pc. We implicitly
include the precessing disk by forcing the disk radiation field to precess
around a symmetry axis with a given period () and a tilt angle ().
We study time evolution of the flows irradiated by the disk, and investigate
basic dependencies of the flow morphology, mass flux, angular momentum on
different combinations of and . We find the gas flow settles into a
configuration with two components, (1) an equatorial inflow and (2) a bipolar
inflow/outflow with the outflow leaving the system along the poles (the
directions of disk normals). However, the flow does not always reach a steady
state. We find that the maximum outflow velocity and the kinetic outflow power
at the outer boundary can be reduced significantly with increasing . We
also find that of the mass inflow rate across the inner boundary does not
change significantly with increasing . (Abbreviated)Comment: Accepted for publication in ApJ. 15 pages, 7 figures. A version with
full resolution figures can be downloaded from
http://www.physics.unlv.edu/~rk/preprint/precess.pd
Sheared Flow As A Stabilizing Mechanism In Astrophysical Jets
It has been hypothesized that the sustained narrowness observed in the
asymptotic cylindrical region of bipolar outflows from Young Stellar Objects
(YSO) indicates that these jets are magnetically collimated. The j cross B
force observed in z-pinch plasmas is a possible explanation for these
observations. However, z-pinch plasmas are subject to current driven
instabilities (CDI). The interest in using z-pinches for controlled nuclear
fusion has lead to an extensive theory of the stability of magnetically
confined plasmas. Analytical, numerical, and experimental evidence from this
field suggest that sheared flow in magnetized plasmas can reduce the growth
rates of the sausage and kink instabilities. Here we propose the hypothesis
that sheared helical flow can exert a similar stabilizing influence on CDI in
YSO jets.Comment: 13 pages, 2 figure
Global asymptotic solutions for relativistic MHD jets and winds
We consider relativistic, stationary, axisymmetric, polytropic, unconfined,
perfect MHD winds, assuming their five lagrangian first integrals to be known.
The asymptotic structure consists of field-regions bordered by boundary layers
along the polar axis and at null surfaces, such as the equatorial plane, which
have the structure of charged column or sheet pinches supported by plasma or
magnetic poloidal pressure. In each field-region cell, the proper current
(defined here as the ratio of the asymptotic poloidal current to the asymptotic
Lorentz factor) remains constant. Our solution is given in the form of matched
asymptotic solutions separately valid outside and inside the boundary layers.
An Hamilton-Jacobi equation, or equivalently a Grad-Shafranov equation, gives
the asymptotic structure in the field-regions of winds which carry Poynting
flux to infinity. An important consistency relation is found to exist between
axial pressure, axial current and asymptotic Lorentz factor. We similarly
derive WKB-type analytic solutions for winds which are kinetic-energy dominated
at infinity and whose magnetic surfaces focus to paraboloids. The density on
the axis in the polar boundary column is shown to slowly fall off as a negative
power of the logarithm of the distance to the wind source. The geometry of
magnetic surfaces in all parts of the asymptotic domain, including boundary
layers, is explicitly deduced in terms of the first-integrals.Comment: 39 pages, 7 figures, accepted for publication in Ap
Magnetic Field Effects on the Structure and Evolution of Overdense Radiatively Cooling Jets
We investigate the effect of magnetic fields on the propagation dynamics and
morphology of overdense, radiatively cooling, supermagnetosonic jets, with the
help of fully three-dimensional SPMHD simulations. Evaluated for a set of
parameters which are mainly suitable for protostellar jets (with density ratios
between the jet and the ambient medium 3-10, and ambient Mach number ~ 24),
these simulations are also compared with baseline non-magnetic and adiabatic
calculations. We find that, after amplification by compression and
re-orientation in nonparallel shocks at the working surface, the magnetic field
that is carried backward with the shocked gas into the cocoon improves the jet
collimation relative to the purely hydrodynamic (HD) systems. Low-amplitude,
approximately equally spaced internal shocks (which are absent in the HD
systems) are produced by MHD K-H reflection pinch modes. The longitudinal field
geometry also excites non-axisymmetric helical modes which cause some beam
wiggling. The strength and amount of these modes are, however, reduced (by ~
twice) in the presence of radiative cooling relative to the adiabatic cases.
Besides, a large density ratio between the jet and the ambient medium also
reduces, in general, the number of the internal shocks. As a consequence, the
weakness of the induced internal shocks makes it doubtful that the magnetic
pinches could produce by themselves the bright knots observed in the overdense,
radiatively cooling protostellar jets.Comment: To appear in ApJ; 36 pages + 16 (gif) figures. PostScript files of
figures are available at http://www.iagusp.usp.br/preprints/preprint.htm
The Propagation of Magneto-Centrifugally Launched Jets: I
We present simulations of the propagation of magnetized jets. This work
differs from previous studies in that the cross-sectional distributions of the
jets's state variables are derived from analytical models for
magneto-centrifugal launching. The source is a magnetized rotator whose
properties are specfied as boundary conditions. The jets in these simulations
are considerably more complex than the ``top-hat''constant density etc.
profiles used in previous work. We find that density and magnetic field
stratification (with radius) in the jet leads to new behavior including the
separation of an inner jet core from a low density collar. We find this {\it
jet within a jet} structure, along with the magnetic stresses, leads to
propagation behaviors not observed in previous simulation studies. Our
methodology allows us to compare MHD jets from different types of sources whose
properties could ultimately be derived from the behavior of the propagating
jets.Comment: 42 pages, accepted by the Ap
A Sample of Low Redshift BL Lacs. I. The Radio Data
We present a new sample of 30 nearby (z<0.2) BL Lacs, selected to study the
nuclear as well as the large scale properties of low power radio sources. In
this first paper, we show and discuss new radio data taken with the VLA (19
objects at 1.4 GHz, either in A or C configuration, or both) as well as with
the VLBA (15 sources at 5 GHz). On the kiloparsec scale, all objects exhibit a
compact core and a variety of radio morphologies (jets, halos, secondary
compact components). On the parsec scale, we find weak cores and a few short,
one-sided, jets. From the jet/counter-jet ratio, core dominance, and
synchrotron self Compton model we estimate the intrinsic orientation and
velocity of the jets. The resulting properties of BL Lacs are similar to those
of a parent population composed of FR I radio galaxies.Comment: 46 pages, 12 figures, accepted for publication in Ap
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