22 research outputs found
Spallative ablation of dielectrics by X-ray laser
Short laser pulse in wide range of wavelengths, from infrared to X-ray,
disturbs electron-ion equilibrium and rises pressure in a heated layer. The
case where pulse duration is shorter than acoustic relaxation time
is considered in the paper. It is shown that this short pulse may cause
thermomechanical phenomena such as spallative ablation regardless to
wavelength. While the physics of electron-ion relaxation on wavelength and
various electron spectra of substances: there are spectra with an energy gap in
semiconductors and dielectrics opposed to gapless continuous spectra in metals.
The paper describes entire sequence of thermomechanical processes from
expansion, nucleation, foaming, and nanostructuring to spallation with
particular attention to spallation by X-ray pulse
Two-temperature relaxation and melting after absorption of femtosecond laser pulse
The theory and experiments concerned with the electron-ion thermal relaxation
and melting of overheated crystal lattice constitute the subject of this paper.
The physical model includes two-temperature equation of state, many-body
interatomic potential, the electron-ion energy exchange, electron thermal
conductivity, and optical properties of solid, liquid, and two phase
solid-liquid mixture. Two-temperature hydrodynamics and molecular dynamics
codes are used. An experimental setup with pump-probe technique is used to
follow evolution of an irradiated target with a short time step 100 fs between
the probe femtosecond laser pulses. Accuracy of measurements of reflection
coefficient and phase of reflected probe light are ~1% and \sim 1\un{nm},
respectively. It is found that,
{\it firstly}, the electron-electron collisions make a minor contribution to
a light absorbtion in solid Al at moderate intensities;
{\it secondly}, the phase shift of a reflected probe results from heating of
ion subsystem and kinetics of melting of Al crystal during 0
where is time delay between the pump and probe pulses measured from the
maximum of the pump;
{\it thirdly} the optical response of Au to a pump shows a marked contrast to
that of Al on account of excitation of \textit{d}-electronsComment: 6th International Conference on Photo-Excited Processes and
Applications 9-12 Sep 2008, Sapporo, Japan, http://www.icpepa6.com, the
contributed paper will be published in Applied Surface Science(2009
Equilibration processes in the Warm-Hot Intergalactic Medium
The Warm-Hot Intergalactic Medium (WHIM) is thought to contribute about 40-50
% to the baryonic budget at the present evolution stage of the universe. The
observed large scale structure is likely to be due to gravitational growth of
density fluctuations in the post-inflation era. The evolving cosmic web is
governed by non-linear gravitational growth of the initially weak density
fluctuations in the dark energy dominated cosmology. Non-linear structure
formation, accretion and merging processes, star forming and AGN activity
produce gas shocks in the WHIM. Shock waves are converting a fraction of the
gravitation power to thermal and non-thermal emission of baryonic/leptonic
matter. They provide the most likely way to power the luminous matter in the
WHIM. The plasma shocks in the WHIM are expected to be collisionless.
Collisionless shocks produce a highly non-equilibrium state with anisotropic
temperatures and a large differences in ion and electron temperatures. We
discuss the ion and electron heating by the collisionless shocks and then
review the plasma processes responsible for the Coulomb equilibration and
collisional ionisation equilibrium of oxygen ions in the WHIM. MHD-turbulence
produced by the strong collisionless shocks could provide a sizeable
non-thermal contribution to the observed Doppler parameter of the UV line
spectra of the WHIM.Comment: 13 pages, 4 figures, accepted for publication in Space Science
Reviews, special issue "Clusters of galaxies: beyond the thermal view",
Editor J.S. Kaastra, Chapter 8; work done by an international team at the
International Space Science Institute (ISSI), Bern, organised by J.S.
Kaastra, A.M. Bykov, S. Schindler & J.A.M. Bleeke
Particle acceleration mechanisms
We review the possible mechanisms for production of non-thermal electrons
which are responsible for non-thermal radiation in clusters of galaxies. Our
primary focus is on non-thermal Bremsstrahlung and inverse Compton scattering,
that produce hard X-ray emission. We briefly review acceleration mechanisms and
point out that in most astrophysical situations, and in particular for the
intracluster medium, shocks, turbulence and plasma waves play a crucial role.
We consider two scenarios for production of non-thermal radiation. The first is
hard X-ray emission due to non-thermal Bremsstrahlung by nonrelativistic
particles. Non-thermal tails are produced by accelerating electrons from the
background plasma with an initial Maxwellian distribution. However, these tails
are accompanied by significant heating and they are present for a short time of
<10^6 yr, which is also the time that the tail will be thermalised. Such
non-thermal tails, even if possible, can only explain the hard X-ray but not
the radio emission which needs GeV or higher energy electrons. For these and
for production of hard X-rays by the inverse Compton model, we need the second
scenario where there is injection and subsequent acceleration of relativistic
electrons. It is shown that a steady state situation, for example arising from
secondary electrons produced from cosmic ray proton scattering by background
protons, will most likely lead to flatter than required electron spectra or it
requires a short escape time of the electrons from the cluster. An episodic
injection of relativistic electrons, presumably from galaxies or AGN, and/or
episodic generation of turbulence and shocks by mergers can result in an
electron spectrum consistent with observations but for only a short period of
less than one billion years.Comment: 22 pages, 5 figures, accepted for publication in Space Science
Reviews, special issue "Clusters of galaxies: beyond the thermal view",
Editor J.S. Kaastra, Chapter 11; work done by an international team at the
International Space Science Institute (ISSI), Bern, organised by J.S.
Kaastra, A.M. Bykov, S. Schindler & J.A.M. Bleeke
Non-thermal processes in cosmological simulations
Non-thermal components are key ingredients for understanding clusters of
galaxies. In the hierarchical model of structure formation, shocks and
large-scale turbulence are unavoidable in the cluster formation processes.
Understanding the amplification and evolution of the magnetic field in galaxy
clusters is necessary for modelling both the heat transport and the dissipative
processes in the hot intra-cluster plasma. The acceleration, transport and
interactions of non-thermal energetic particles are essential for modelling the
observed emissions. Therefore, the inclusion of the non-thermal components will
be mandatory for simulating accurately the global dynamical processes in
clusters. In this review, we summarise the results obtained with the
simulations of the formation of galaxy clusters which address the issues of
shocks, magnetic field, cosmic ray particles and turbulence.Comment: 27 pages, 16 figures, accepted for publication in Space Science
Reviews, special issue "Clusters of galaxies: beyond the thermal view",
Editor J.S. Kaastra, Chapter 15; work done by an international team at the
International Space Science Institute (ISSI), Bern, organised by J.S.
Kaastra, A.M. Bykov, S. Schindler & J.A.M. Bleeke
Electron-ion energy exchange in simple metals in Ziman approach
© Published under licence by IOP Publishing Ltd. The coefficient of the electron-ion energy exchange in liquid aluminum is calculated within the framework of Ziman approach for electron kinetic coefficients. Calculations are made to study dependence of the electron-ion heat transfer coefficient on the electron and ion temperatures
Analytic description of five-minute oscillations of the sun
Dynamics of perturbations in atmospheres of planets and in stars have been considered. An analytical description of the spectra of frequences of oscillations and increments of dynamic instabilities has been found for the law of power distributions of thermodynamic quantities in the plane case. A polytropic approximation is widely used in astrophysics. In this case an entropy distribution near the surface r=r_s of a star is a power distribution S=const_s (r_s-r)"#theta#. The exponent #theta# is a function of the polytropic index N and the adiabatic exponent #gamma#[#theta#=1-N(#gamma#-1)]. The density distributions is (r_s-r)"N. The previously known classical case with homogeneous density (#theta#=1 N=0) for spherical geometry, was considered by Pekeris, 1938 (see, e.g., Ledoux, 1958, paragraph 76 or Cox, 1980, paragraph 17.7) and the solution for homogeneous plane distribution of entropy (#theta#=0, N=1/(#gamma#-1)). Here the spectral solution for the case of the general polytrope in plane geometry with arbitrary values of N and #theta# will be presented. It appears, that this problem is closely connected with Schroedinger's equation with a Coulomb potential. Eigenfunctions are expressed in terms of confluent hypergeometric functions. In the case of spatially invariant boundary conditions the spectrum is split into pairs of acoustic and gravity modes. This duality means that for every mode number n there is one acoustic and one gravity mode. Their frequencies are different but the eigenfunctions of the Lagrangian pressure variation for these modes are identical. A comparison with five-minute oscillations of the Sun is made. It is shown that the obtained analytic expressions describe these oscillations rather well. (orig.)SIGLEAvailable from TIB Hannover: RR 4697(956) / FIZ - Fachinformationszzentrum Karlsruhe / TIB - Technische InformationsbibliothekDEGerman