174 research outputs found
PIERNIK mhd code - a multi-fluid, non-ideal extension of the relaxing-TVD scheme (I)
We present a new multi-fluid, grid MHD code PIERNIK, which is based on the
Relaxing TVD scheme. The original scheme has been extended by an addition of
dynamically independent, but interacting fluids: dust and a diffusive cosmic
ray gas, described within the fluid approximation, with an option to add other
fluids in an easy way. The code has been equipped with shearing-box boundary
conditions, and a selfgravity module, Ohmic resistivity module, as well as
other facilities which are useful in astrophysical fluid-dynamical simulations.
The code is parallelized by means of the MPI library. In this paper we shortly
introduce basic elements of the Relaxing TVD MHD algorithm, following Trac &
Pen (2003) and Pen et al. (2003), and then focus on the conservative
implementation of the shearing box model, constructed with the aid of the
Masset's (2000) method. We present results of a test example of a formation of
a gravitationally bounded object (planet) in a self-gravitating and
differentially rotating fluid.Comment: 6 pages, 3 figures, conference proceedings of the Torun Exoplanets
200
Cosmic-ray driven dynamo in galaxies
We present recent developments of global galactic-scale numerical models of
the Cosmic Ray (CR) driven dynamo, which was originally proposed by Parker
(1992). We conduct a series of direct CR+MHD numerical simulations of the
dynamics of the interstellar medium (ISM), composed of gas, magnetic fields and
CR components. We take into account CRs accelerated in randomly distributed
supernova (SN) remnants, and assume that SNe deposit small-scale, randomly
oriented, dipolar magnetic fields into the ISM. The amplification timescale of
the large-scale magnetic field resulting from the CR-driven dynamo is
comparable to the galactic rotation period. The process efficiently converts
small-scale magnetic fields of SN-remnants into galactic-scale magnetic fields.
The resulting magnetic field structure resembles the X-shaped magnetic fields
observed in edge-on galaxies.Comment: 6 pages, 4 figures, to appear in Proceedings of IAU Symp. 274,
Advances in Plasma Astrophysics, ed. A. Bonanno, E. de Gouveia dal Pino and
A. Kosoviche
Kelvin-Helmholtz instability of relativistic jets - the transition from linear to nonlinear regime
The observed wiggles and knots in astrophysical jets as well as the
curvilinear motion of radio emitting features are frequently interpreted as
signatures of the Kelvin-Helmholtz (KH) instability (eg. Hardee 1987). We
investigate the KH instability of a hydrodynamic jet composed of a relativistic
gas, surrounded by a nonrelativistic external medium and moving with a
relativistic bulk speed. We show basic nonlinear effects, which become
important for a finite amplitude KH modes. Since the KH instability in
supersonic jets involves acoustic waves over-reflected on jet boundaries, the
basic nonlinear effect relies on the steepening of the acoustic wave fronts,
leading to the formation of shocks. It turns our that the shocks appear
predominantly in the external nonrelativistic gas, while the internal acoustic
waves remain linear for a much longer time. In addition, the external medium
"hardens" as soon as the boundary oscillation velocity becomes comparable to
the external sound speed. On the other hand, the amplification of internal
waves due to the over-reflection is limited by a nonlinearity of the Lorentz
factor. This implies that the sidereal oscillations of the jet
boundary, resulting from the K-H instability, are limited to very small
amplitudes comparable to a fraction of the jet radius.Comment: TeX, 5 pages, no figures, lecproc.cmm included, To appear in
Proceedings of ``Relativistic jets in AGNs'', Krakow, Poland, 27-30 May 1997,
M.Ostrowski, M.Sikora, G.Madejski, M. Begelman (eds.
The galactic dynamo effect due to Parker-shearing instability of magnetic flux tubes. II. Numerical simulations and the nonlinear evolution
In this paper we continue investigations of the Parker-shearing instability
performing numerical simulations of the magnetic flux tube dynamics in the thin
flux-tube approximation. We show that evolution of flux tubes resulting from
numerical simulations is very similar to that of linear solutions if the
vertical displacements are smaller than the vertical scale height of the
galactic disc. If the vertical displacements are comparable to , the
vertical growth of perturbations is faster in the nonlinear range than in the
linear one and we observe a rapid inflation of the flux tube at its top, which
leads to a singularity in numerical simulations, if only the cosmic rays are
taken into account. Then we perform simulations for the case of nonuniform
external medium, which show that the dominating wavelength of the Parker
instability is the same as the wavelength of modulations of external medium. As
a consequence of this fact, in the case of dominating cosmic ray pressure, the
dynamo effect related to these short wavelength modulations is much
more efficient than that related to the linearly most unstable long wavelengths
modes of the Parker instability. Under the influence of differential forces
resulting from differential rotation and the density waves, the -effect
is essentially magnified in the spiral arms and diminished in the interarm
regions, what confirms our previous results obtained in the linear
approximation.Comment: LaTeX, 13 pages, 15 ps figures, uses l-aa.sty and epsf.sty. Published
in Astronomy & Astrophysics, 327, 81
Parker-Jeans Instability of Gaseous Disks Including the Effect of Cosmic Rays
We use linear analysis to examine the effect of cosmic rays (CRs) on the
Parker-Jeans instability of magnetized self-gravitating gaseous disks. We adopt
a slab equilibrium model in which the gravity (including self-gravity) is
perpendicular to the mid-plane, the magnetic field lies along the slab. CR is
described as a fluid and only along magnetic field lines diffusion is
considered. The linearised equations are solved numerically. The system is
susceptible to Parker-Jeans instability. In general the system is less unstable
when the CR diffusion coefficient is smaller (i.e., the coupling between the
CRs and plasma is stronger). The system is also less unstable if CR pressure is
larger. This is a reminiscence of the fact that Jeans instability and Parker
instability are less unstable when the gas pressure is larger (or temperature
is higher). Moreover, for large CR diffusion coefficient (or small CR
pressure), perturbations parallel to the magnetic field are more unstable than
those perpendicular to it. The other governing factor on the growth rate of the
perturbations in different directions is the thickness of the disk or the
strength of the external pressure on the disk. In fact, this is the determining
factor in some parameter regimes.Comment: 19pages, 14figures submitted to Ap
The galactic dynamo effect due to Parker-shearing instability of magnetic flux tubes. I. General formalism and the linear approximation
In this paper we investigate the idea of Hanasz & Lesch 1993 that the
galactic dynamo effect is due to the Parker instability of magnetic flux tubes.
In addition to the former approach, we take into account more general physical
conditions in this paper, by incorporating cosmic rays and differential forces
due to the axisymmetric differential rotation and the density waves as well. We
present the theory of slender magnetic flux tube dynamics in the thin flux tube
approximation and the Lagrange description. This is the application of the
formalism obtained for solar magnetic flux tubes by Spruit (1981), to the
galactic conditions. We perform a linear stability analysis for the
Parker-shearing instability of magnetic flux tubes in galactic discs and then
calculate the dynamo coefficients. We present a number of new effects which are
very essential for cosmological and contemporary evolution of galactic magnetic
fields. First of all we demonstrate that a very strong dynamo -effect
is possible in the limit of weak magnetic fields in presence of cosmic rays.
Second, we show that the differential force resulting from axisymmetric
differential rotation and the linear density waves causes that the
-effect is essentially magnified in galactic arms and switched off in
the interarm regions. Moreover, we predict a non-uniform magnetic field in
spiral arms and well aligned one in interarm regions. These properties are well
confirmed by recent observational results by Beck & Hoernes (1996)Comment: LaTeX, 15 pages, 8 figures, uses l-aa.sty and epsf.sty, minor
corrections to match the published version, Published in Astronomy &
Astrophysics, 321, 100
Initial Magnetization of Galaxies by Exploding, Magnetized Stars
We conduct a series of magnetohydrodynamical (MHD) simulations of magnetized
interstellar medium (ISM) disturbed by exploding stars. Each star deposits a
randomly oriented, dipolar magnetic field into ISM. The simulations are
performed in a Cartesian box, in a reference frame that is corotating with the
galactic disk. The medium is stratified by vertical galactic gravity. The
resulting turbulent state of ISM magnetized by the stellar explosions is
processed with the aid of Fourier analysis. The results leads to the conclusion
that the input of magnetic energy from exploding stars is additionally
multiplied by differential rotation. The resulting magnetic field appears to
grow up in small-scale component, while the total magnetic flux remains
limited. Our results indicate that magnetic field originating from exploding
stars can be a source of initial magnetic fields for a subsequent dynamo
process.Comment: Published in Proceedings of the 14th Young Scientists Conference on
Astronomy and Space Physics, Kyiv, Ukraine, April 23-28, 200
Hydrodynamical instability of extragalactic stratified jets
The recent development of tomographic analysis of radio data shows the
presence of sheaths around several extragalactic jets. We have studied the
Kelvin-Helmholtz instability of such stratified jets, describing them as inner
relativistic beams embedded in slower plasma envelopes. We find that the para-
meters of the envelope generally determine the Kelvin-Helmholtz properties of
the jet which thus appears isolated from any ambient external medium.Comment: LaTeX, 5 pages, 1 figure and crckapb.sty, epsf.sty included, To
appear in the proceedings of Girona Conference ``Blazars, Black Holes and
Jets'', 9-12 September 1996, Girona, Spai
Cosmic-ray driven dynamo in galactic disks
We present new developments on the Cosmic--Ray driven, galactic dynamo,
modeled by means of direct, resistive CR--MHD simulations, performed with ZEUS
and PIERNIK codes. The dynamo action, leading to the amplification of
large--scale galactic magnetic fields on galactic rotation timescales, appears
as a result of galactic differential rotation, buoyancy of the cosmic ray
component and resistive dissipation of small--scale turbulent magnetic fields.
Our new results include demonstration of the global--galactic dynamo action
driven by Cosmic Rays supplied in supernova remnants. An essential outcome of
the new series of global galactic dynamo models is the equipartition of the gas
turbulent energy with magnetic field energy and cosmic ray energy, in saturated
states of the dynamo on large galactic scales.Comment: 6 pages, 3 figures, To be published in "Cosmic Magnetic Fields: From
Planets, to Stars and Galaxies", K.G. Strassmeier, A.G. Kosovichev & J.E.
Beckman, eds., Proc. IAU Symp. 259, CU
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