250 research outputs found
Turbulent Contributions to Ohm's Law in Axisymmetric Magnetized Plasmas
The effect of magnetic turbulence in shaping the current density in
axisymmetric magnetized plasma is analyzed using a turbulent extension of Ohm's
law derived from the self-consistent action-angle transport theory. Besides the
well-known hyper-resistive (helicity-conserving) contribution, the generalized
Ohm's law contains an anomalous resistivity term, and a turbulent
bootstrap-like term proportional to the current density derivative. The
numerical solution of the equation for equilibrium and turbulence profiles
characteristic of conventional and advanced scenarios shows that, trough
"turbulent bootstrap" effect and anomalous resistivity turbulence can generate
power and parallel current which are a sizable portion (about 20-25%) of the
corresponding effects associated with the neoclassical bootstrap effect. The
degree of alignment of the turbulence peak and the pressure gradient plays an
important role in defining the steady-state regime. In fully bootstrapped
tokamak, the hyper-resistivity is essential in overcoming the intrinsic
limitation of the hollow current profile.Comment: 19 pages, 6 figures, journal pape
A Jupiter-mass planet around the K0 giant HD 208897
For over 10 years, we have carried out a precise radial velocity (RV) survey
to find substellar companions around evolved G,K-type stars to extend our
knowledge of planet formation and evolution. We performed high precision RV
measurements for the giant star HD 208897 using an iodine (I2) absorption cell.
The measurements were made at T\"UB\.ITAK National Observatory (TUG, RTT150)
and Okayama Astrophysical Observatory (OAO). For the origin of the periodic
variation seen in the RV data of the star, we adopted a Keplerian motion caused
by an unseen companion. We found that the star hosts a planet with a minimum
mass of m2sini=1.40MJ, which is relatively low compared to those of known
planets orbiting evolved intermediate-mass stars. The planet is in a nearly
circular orbit with a period of P=353 days at about 1 AU distance from the host
star. The star is metal rich and located at the early phase of ascent along the
red giant branch. The photometric observations of the star at Ankara University
Kreiken Observatory (AUKR) and the HIPPARCOS photometry show no sign of
variation with periods associated with the RV variation. Neither bisector
velocity analysis nor analysis of the Ca II and Halpha lines shows any
correlation with the RV measurements
Magnetic Field Limitations on Advection Dominated Flows
Recent papers discussing advection dominated accretion flows (ADAF) as a
solution for astrophysical accretion problems should be treated with some
caution because of their uncertain physical basis. The suggestions underlying
ADAF involve ignoring the magnetic field reconnection in heating of the plasma
flow, assuming electron heating due only to binary Coulomb collisions with
ions. Here, we analyze the physical processes in optically thin accretion flows
at low accretion rates including the influence of an equipartition turbulent
magnetic field. For these conditions there is continuous destruction of
magnetic flux by reconnection.
The reconnection is expected to significantly heat the electrons which can
efficiently emit magnetobremstrahlung radiation. Because of this electron
emission, the radiative efficiency of the ADAF is not small. We suggest that
the small luminosities of nearby galactic black holes is due to outflows rather
than ADAF accretion.Comment: 7 pages, 3 figures, Submitted to Ap
Shock Acceleration of Cosmic Rays - a critical review
Motivated by recent unsuccessful efforts to detect the predicted flux of TeV
gamma-rays from supernova remnants, we present a critical examination of the
theory on which these predictions are based. Three crucial problems are
identified: injection, maximum achievable particle energy and spectral index.
In each case significant new advances in understanding have been achieved,
which cast doubt on prevailing paradigms such as Bohm diffusion and
single-fluid MHD. This indicates that more realistic analytical models, backed
by more sophisticated numerical techniques should be employed to obtain
reliable predictions. Preliminary work on incorporating the effects of
anomalous transport suggest that the resulting spectrum should be significantly
softer than that predicted by conventional theory.Comment: 8 pages, invited review presented at the 17th ECRS, Lodz, July 2000;
to appear in Journal of Physics G: Nuclear and Particle Physic
Diffusion Time-Scale Invariance, Markovization Processes and Memory Effects in Lennard-Jones Liquids
We report the results of calculation of diffusion coefficients for
Lennard-Jones liquids, based on the idea of time-scale invariance of relaxation
processes in liquids. The results were compared with the molecular dynamics
data for Lennard-Jones system and a good agreement of our theory with these
data over a wide range of densities and temperatures was obtained. By
calculations of the non-Markovity parameter we have estimated numerically
statistical memory effects of diffusion in detail.Comment: 10 pages, 3 figure
The Boltzmann equation for colourless plasmons in hot QCD plasma. Semiclassical approximation
Within the framework of the semiclassical approximation, we derive the
Boltzmann equation describing the dynamics of colorless plasmons in a hot QCD
plasma. The probability of the plasmon-plasmon scattering at the leading order
in the coupling constant is obtained. This probability is gauge-independent at
least in the class of the covariant and temporal gauges. It is noted that the
structure of the scattering kernel possesses important qualitative difference
from the corresponding one in the Abelian plasma, in spite of the fact that we
focused our study on the colorless soft excitations. It is shown that
four-plasmon decay is suppressed by the power of relative to the process of
nonlinear scattering of plasmons by thermal particles at the soft momentum
scale. It is stated that the former process becomes important in going to the
ultrasoft region of the momentum scale.Comment: 41, LaTeX, minor changes, identical to published versio
Magnetohydrodynamics and Plasma Cosmology
We study the linear magnetohydrodynamic (MHD) equations, both in the
Newtonian and the general-relativistic limit, as regards a viscous magnetized
fluid of finite conductivity and discuss instability criteria. In addition, we
explore the excitation of cosmological perturbations in anisotropic spacetimes,
in the presence of an ambient magnetic field. Acoustic, electromagnetic (e/m)
and fast-magnetosonic modes, propagating normal to the magnetic field, can be
excited, resulting in several implications of cosmological significance.Comment: 9 pages, RevTeX, To appear in the Proceedings of the Peyresq X
Meeting, IJTP Conference Serie
A Jupiter-mass planet around the K0 giant HD 208897
© ESO, 2017. For over 10 years, we have carried out a precise radial velocity (RV) survey to find substellar companions around evolved G, K-type stars to extend our knowledge of planet formation and evolution. We performed high precision RV measurements for the giant star HD 208897 using an iodine (I 2 ) absorption cell. The measurements were made at TÜBA TAK National Observatory (TUG; RTT150) and Okayama Astrophysical Observatory (OAO). For the origin of the periodic variation seen in the RV data of the star, we adopted a Keplerian motion caused by an unseen companion. We found that the star hosts a planet with a minimum mass of m 2 sini = 1.40 M J , which is relatively low compared to those of known planets orbiting evolved intermediate-mass stars. The planet is in a nearly circular orbit with a period of P = 353 days at about 1 AU distance from the host star. The star is metal rich and located at the early phase of ascent along the red giant branch. The photometric observations of the star at Ankara University Kreiken Observatory (AUKR) and the Hipparcos photometry show no sign of variation with periods associated with the RV variation. Neither bisector velocity analysis nor analysis of the Ca II and Hα lines shows any correlation with the RV measurements
Jet disc coupling in black hole binaries
In the last decade multi-wavelength observations have demonstrated the
importance of jets in the energy output of accreting black hole binaries. The
observed correlations between the presence of a jet and the state of the
accretion flow provide important information on the coupling between accretion
and ejection processes. After a brief review of the properties of black hole
binaries, I illustrate the connection between accretion and ejection through
two particularly interesting examples. First, an INTEGRAL observation of Cygnus
X-1 during a 'mini-' state transition reveals disc jet coupling on time scales
of orders of hours. Second, the black hole XTEJ1118+480 shows complex
correlations between the X-ray and optical emission. Those correlations are
interpreted in terms of coupling between disc and jet on time scales of seconds
or less. Those observations are discussed in the framework of current models.Comment: Invited talk at the Fifth Stromlo Symposium: Disks, Winds & Jets -
from Planets to Quasars. Accepted for publication in Astrophysics & Space
Scienc
Low mass stellar companions around four giant stars
We present three low-mass and one solar mass companions found around four intermediate-mass giants HD1695, HD120235, HD145316 and HD200004 from precise radial velocity measurements using the 1.5 m Russian-Turkish Telescope (RTT150) at the TÜBITAK National Observatory of Turkey (TUG). The stellar parameters, which are effective temperature (Teff), surface gravity (logg) and metallicity ([Fe/H]), as well as rotational velocity (vsini) are obtained from spectral analysis. From the estimated stellar masses, the orbital parameters of the companions are also derived. We find two types of Keplerian solutions for the companion of HD120235: (1) periods 5522 days and eccentricity of e∼0.93, and (2) periods 1566 days and eccentricity of e∼0.83. From the abundances analysis HD1695 is found to be a metal-rich star with [Fe/H]>0.1, while HD200004 is a metal poor star with [Fe/H]<-0.2. The other two stars, HD120235 and HD145316, have solar-like abundances with [Fe/H]∼0.0. Our stellar parameters and orbital solutions show that all of these stars are evolved intermediate-mass giants. © 2014 Elsevier B.V. All rights reserved
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