共查询到20条相似文献，搜索用时 31 毫秒
1.
The non-thermal shielding effects on the inverse Compton scattering are investigated in astrophysical non-thermal Lorentzian plasmas. The inverse Compton power is obtained by the modified Compton scattering cross section in Lorentzian plasmas with the blackbody photon distribution. The total Compton power is also obtained by the Lorentzan distribution of plasmas. It is found that the influence of non-thermal character of the plasma suppresses the inverse Compton power in astrophysical Lorentzian plasmas. It is also found that the non-thermal effect on the inverse Compton power decreases with an increase of the temperature. In addition, the non-thermal effect on the total Compton power with Lorentzan plasmas increases in low-temperature photons and, however, decreases in intermediate-temperature photons with increasing Debye length. The variation of the total Compton power is also discussed. 相似文献
2.
There are several astrophysical situations where one needs to study the dynamics of magnetic flux in partially ionized turbulent plasmas. In a partially ionized plasma, the magnetic induction is subjected to the ambipolar diffusion and the Hall effect in addition to the usual resistive dissipation. In this paper, we initiate the study of the kinematic dynamo in a partially ionized turbulent plasma. The Hall effect arises from the treatment of the electrons and the ions as two separate fluids and the ambipolar diffusion due to the inclusion of neutrals as the third fluid. It is shown that these non-ideal effects modify the so-called α effect and the turbulent diffusion coefficient β in a rather substantial way. The Hall effect may enhance or quench the dynamo action altogether. The ambipolar diffusion brings in an α which depends on the mean magnetic field. The new correlations embodying the coupling of the charged fluids and the neutral fluid appear in a decisive manner. The turbulence is necessarily magnetohydrodynamic with new spatial and time-scales. The nature of the new correlations is demonstrated by taking the Alfvénic turbulence as an example. 相似文献
3.
The present review concerns the relevance of collisionless reconnection in the astrophysical context. Emphasis is put on recent developments in theory obtained from collisionless numerical simulations in two and three dimensions. It is stressed that magnetic reconnection is a universal process of particular importance under collisionless conditions, when both collisional and anomalous dissipation are irrelevant. While collisional (resistive) reconnection is a slow, diffusive process, collisionless reconnection is spontaneous. On any astrophysical time scale, it is explosive. It sets on when electric current widths become comparable to the leptonic inertial length in the so-called lepton (electron/positron) “diffusion region”, where leptons de-magnetise. Here, the magnetic field contacts its oppositely directed partner and annihilates. Spontaneous reconnection breaks the original magnetic symmetry, violently releases the stored free energy of the electric current, and causes plasma heating and particle acceleration. Ultimately, the released energy is provided by mechanical motion of either the two colliding magnetised plasmas that generate the current sheet or the internal turbulence cascading down to lepton-scale current filaments. Spontaneous reconnection in such extended current sheets that separate two colliding plasmas results in the generation of many reconnection sites (tearing modes) distributed over the current surface, each consisting of lepton exhausts and jets which are separated by plasmoids. Volume-filling factors of reconnection sites are estimated to be as large as \({<}10^{-5}\) per current sheet. Lepton currents inside exhausts may be strong enough to excite Buneman and, for large thermal pressure anisotropy, also Weibel instabilities. They bifurcate and break off into many small-scale current filaments and magnetic flux ropes exhibiting turbulent magnetic power spectra of very flat power-law shape \(W_b\propto k^{-\alpha }\) in wavenumber k with power becoming as low as \(\alpha \approx 2\). Spontaneous reconnection generates small-scale turbulence. Imposed external turbulence tends to temporarily increase the reconnection rate. Reconnecting ultra-relativistic current sheets decay into large numbers of magnetic flux ropes composed of chains of plasmoids and lepton exhausts. They form highly structured current surfaces, “current carpets”. By including synchrotron radiation losses, one favours tearing-mode reconnection over the drift-kink deformation of the current sheet. Lepton acceleration occurs in the reconnection-electric field in multiple encounters with the exhausts and plasmoids. This is a Fermi-like process. It results in power-law tails on the lepton energy distribution. This effect becomes pronounced in ultra-relativistic reconnection where it yields extremely hard lepton power-law energy spectra approaching \(F(\gamma )\propto \gamma ^{-1}\), with \(\gamma \) the lepton energy. The synchrotron radiation limit becomes substantially exceeded. Relativistic reconnection is a probable generator of current and magnetic turbulence, and a mechanism that produces high-energy radiation. It is also identified as the ultimate dissipation mechanism of the mechanical energy in collisionless magnetohydrodynamic turbulent cascades via lepton-inertial-scale turbulent current filaments. In this case, the volume-filling factor is large. Magnetic turbulence causes strong plasma heating of the entire turbulent volume and violent acceleration via spontaneous lepton-scale reconnection. This may lead to high-energy particle populations filling the whole volume. In this case, it causes non-thermal radiation spectra that span the entire interval from radio waves to gamma rays. 相似文献
4.
C. Hidalgo 《Astrophysics and Space Science》2004,292(1-4):681-690
A view of the mechanisms underlying particle and energy transport in fusion plasmas devices (tokamak and stellarators) is given. The heat and energy transport in fusion plasmas is generally due to turbulent processes. Several driving (plasma gradients) and damping (electric field) mechanisms of turbulence have been investigated. The development of methods to modify and control plasma turbulence by electric field effects has opened a new era on fusion confinement research. Recently, a new approach based on multi-field probability density function statistical analysis has been proposed to describe transport in non-equilibrium systems and to unravel the overall picture connecting transport, gradients and flows in fusion plasmas. 相似文献
5.
Dispersion properties of kinetic Alfvén wave in quantum magnetoplasma are derived. The quantum contribution to the Landau damping of kinetic Alfvén wave is also derived by using linearized Vlasov equation which contains the Bohm quantum potential. Classical Landau damped kinetic Alfvén waves play an important role in turbulence of astrophysical plasmas. The quantum modification in Landau damping of kinetic Alfvén wave can also play a significant role in changing the scaling law of turbulent spectra as well as the formation of damped localized Alfvénic structures in dense astrophysical plasmas. 相似文献
6.
D. B. Melrose 《Astrophysics and Space Science》1996,242(1-2):209-246
Acceleration processes for fast particles in astrophysical and space plasmas are reviewed with emphasis on stochastic acceleration by MHD turbulence and on acceleration by shock waves. Radiation processes in astrophysical and space plasmas are reviewed with emphasis on plasma emission from the solar corona and electron cyclotron maser emission from planets and stars. 相似文献
7.
A short summary of recent progress in measuring and understanding turbulence during magnetic reconnection in laboratory plasmas
is given. Magnetic reconnection is considered as a primary process to dissipate magnetic energy in laboratory and astrophysical
plasmas. A central question concerns why the observed reconnection rates are much faster than predictions made by classical
theories, such as the Sweet–Parker model based on MHD with classical Spitzer resistivity. Often, the local resistivity is
conjectured to be enhanced by turbulence to accelerate reconnection rates either in the context of the Sweet–Parker model
or by facilitating setup of the Pestchek model. Measurements at a dedicated laboratory experiment, called MRX or Magnetic
Reconnection Experiment, have indicated existence of strong electromagnetic turbulence in current sheets undergoing fast reconnection.
The origin of the turbulence has been identified as right-hand polarized whistler waves, propagating obliquely to the reconnecting
field, with a phase velocity comparable to the relative drift velocity. These waves are consistent with an obliquely propagating
electromagnetic lower-hybrid drift instability driven by drift speeds large compared to the Alfven speed in high-beta plasmas.
Interestingly, this instability may explain electromagnetic turbulence also observed in collisionless shocks, which are common
in energetic astrophysical phenomena. 相似文献
8.
A. V. Kolesnichenko 《Solar System Research》2011,45(3):246-263
The problem of the influence of vortex helicity on the synergic structuring of cosmic matter in it, as well as the appearance
of the effect of negative viscosity in three-dimensional gyrotropic turbulence, were studied in the framework of the fundamental
problem of simulating the evolution of a rotating astrophysical nonmagnetic disk—in particular, the accretion disk—surrounding
the Sun at the early stage of its existence. The evolution equations for averaged vorticity and vortex helicity, as well as
rheological relations for the turbulent flow of heat and asymmetrical tensor of the turbulent stress in helical turbulence,
were obtained. The demonstrative dependence of helicity on the rotation velocity, density (temperature) gradients, and turbulent
energy of the disk gas was established. The role of helicity in the appearance of the inverse Richardson-Kolmogorov energy
cascade from small vortices to larger ones and the related process of the generation of the power-consuming macroscale coherent
vortex formations appearing in gyrotropic turbulence at high Reynolds number were discussed. The results of the numerical
experiments confirming the real existence of the inverse energy cascade in helical turbulence were analyzed. It was assumed
that the relatively long-term decay of turbulence in the solar protoplanet cloud can be due to the absence of the reflective
symmetry of the anisotropic field of the turbulent velocities with respect to its equatorial plane. As the concept of the
inverse energy cascade in three-dimensional helical turbulence is more and more reliably confirmed in numerical experiments,
accounting for this effect affecting the structure and dynamics of the astrophysical nonmagnetic disk becomes important during
its simulation. 相似文献
9.
Charge exchange (CX), both onto ions in the solar wind and potentially in other astrophysical contexts, can create X‐ray emission lines largely indistinguishable from those created in collisional or photoionized plasmas. The prime distinguishing characteristic is in the distinctly different line ratios generated by the CX process. A complete astrophysical model of the process would require a vast number of atomic calculations; we describe here an approximate approach that will allow astronomers to evaluate the likely contribution of CX to an observed spectrum. The method relies upon an approximate calculation of the CX cross section paired with detailed atomic structure calculations used to determine the emission lines. Simulated spectra based on observed solar wind CX data are shown for both current (Suzaku) and near‐term (Astro‐H) missions (© 2012 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献
10.
We present the 2-D, two fluid (ions + neutrals) numerical simulations that we are carrying out in order to study the ambipolar filamentation process, in which a magnetized, partially ionized plasma is stirred by turbulence in the ambipolar frequency range. The higher turbulent velocity of the neutrals in the most ionized regions gives rise to a non-linear force driving them out of these regions, and causes the ions and the magnetic flux to condense in the most ionized regions, resulting in a filamentary structure where initial ionization inhomogeneities are amplified. This mechanism might help to explain some features observed in magnetized and partially ionized astrophysical plasmas as the interstellar medium. 相似文献
11.
M. Akbari-Moghanjoughi 《Astrophysics and Space Science》2012,337(2):613-622
Using the extended Poincaré-Lighthill-Kuo (PLK) reductive perturbation method, which incorporates the phase-shift variations,
it is shown that common features on propagation and head-on collisions of ion-acoustic waves exist for a magnetized plasmas
of different inertial-less particle distributions. For instance it is remarked that, the soliton amplitude is always independent
of magnetic field strength while strictly depends on its angle regarding the propagation direction. Both types of solitons
(compressive or rarefactive) are shown to exist which are defined through the critical angle γ=π/2 or other critical values depending on plasma fractional parameters. These critical plasma parameter values also define
the sign of head-on collision phase shift. Furthermore, it is proved that for a given set of plasma parameters there is always
a relative angle of propagation regarding to that of the magnetic-field for which the soliton width is maximum. Current findings
apply to a wide range of magnetized plasmas including those containing background dust ingredients or two-temperature inertial-less
particles and may be used to study laboratory or astrophysical magnetoplasmas. 相似文献
12.
The nonlinear coupling between a large amplitude electromagnetic wave and the slow background motion in a dusty plasma is considered. Stimulated scattering instabilities are investigated. The relevance of our investigation to cometary and astrophysical plasmas is pointed out. 相似文献
13.
Anthony L. Peratt 《Astrophysics and Space Science》1997,256(1-2):51-75
Advances in the simulation of astrophysical and cosmic plasmas are the direct result of advances in computational capabilities, today consisting of new techniques such as multilevel concurrent simulation, multi-teraflop computational platforms and experimental facilities for producing and diagnosing plasmas under extreme conditions for the benchmarking of simulations. Examples of these are the treatment of mesoscalic plasma and the scaling to astrophysical and cosmic dimensions and the Accelerated Strategic Computing Initiative whose goal is to construct petaflop (1015 floating operations per second) computers, and pulsed power and laser inertial confinement plasmas where megajoules of energy are delivered to highly-diagnosed plasmas. This paper concentrates on the achievements to date in simulating and experimentally producing plasmas scaled to both astrophysical and cosmic plasma dimensions. A previous paper (Part I, Peratt, 1997) outlines the algorithms and computational growth. 相似文献
14.
15.
I. M. Hall T. Durmaz R. C. Mancini J. E. Bailey G. A. Rochau 《Astrophysics and Space Science》2011,336(1):189-194
New, high spectral resolution X-ray observations from astrophysical photoionised plasmas have been recorded in recent years
by the Chandra and XMM-Newton orbiting telescopes. These observations provide a wealth of detailed information and have motivated
new efforts at developing a detailed understanding of the atomic kinetics and radiation physics of photoionised plasmas. The
Z facility at Sandia National Laboratories is a powerful source of X-rays that enables us to produce and study photoionised
plasmas in the laboratory under well characterised conditions. We discuss a series of radiation-hydrodynamic simulations to
help understand the X-ray environment, plasma hydrodynamics and atomic kinetics in experiments where a collapsing wire array
at Z is used as an ionising source of radiation to create a photoionised plasma. The numerical simulations are used to investigate
the role that the key experimental parameters have on the photoionised plasma characteristics. 相似文献
16.
S. K. El-Labany E. F. El-Shamy S. K. El-Sherbeny 《Astrophysics and Space Science》2014,351(1):151-158
The oblique collision of nonlinear quantum dust-acoustic (NQDA) solitary waves in a three-dimensional (3D) magnetized dense dusty plasma is investigated. Furthermore, two coupled Kortwege–de Vries equations for describing our model and the analytical phase shifts after the oblique collision of two NQDA solitary waves are derived using the extended Poincaré–Lighthill–Kuo (PLK) method. The modification in the phase shift and the trajectory of the NQDA solitary waves structures due to the inclusion of oblique collision and external magnetic field are discussed numerically. The numerical results are applied to high density astrophysical situations such as in superdense white dwarfs. 相似文献
17.
The head-on collision between two quantum dust-acoustic solitary waves (QDASWs) in ultradense astrophysical objects has been investigated theoretically using the extended Poincaré-Lighthill-Kuo (PLK) method. The Korteweg-de Vries equations and the analytical phase shifts after the head-on collision of the two QDASWs in quantum dusty plasmas are obtained. Numerically, the obtained results demonstrate that the dust size distribution, the quantum corrections of diffraction and the temperatures of electrons and ions have strong effects on the nature of the phase shifts and the trajectories of the two QDASWs after collision. 相似文献
18.
Anthony L. Peratt 《Astrophysics and Space Science》1996,242(1-2):93-163
Plasma science is rich in distinguishable scales ranging from the atomic to the galactic to the meta-galactic, i.e., themesoscale. Thus plasma science has an important contribution to make in understanding the connection between microscopic and macroscopic phenomena. Plasma is a system composed of a large number of particles which interact primarily, but not exclusively, through the electromagnetic field. The problem of understanding the linkages and couplings in multi-scale processes is a frontier problem of modern science involving fields as diverse as plasma phenomena in the laboratory to galactic dynamics.Unlike the first three states of matter, plasma, often called the fourth state of matter, involves the mesoscale and its interdisciplinary founding have drawn upon various subfields of physics including engineering, astronomy, and chemistry. Basic plasma research is now posed to provide, with major developments in instrumentation and large-scale computational resources, fundamental insights into the properties of matter on scales ranging from the atomic to the galactic. In all cases, these are treated as mesoscale systems. Thus, basic plasma research, when applied to the study of astrophysical and space plasmas, recognizes that the behavior of the near-earth plasma environment may depend to some extent on the behavior of the stellar plasma, that may in turn be governed by galactic plasmas. However, unlike laboratory plasmas, astrophysical plasmas will forever be inaccessible to in situ observation. The inability to test concepts and theories of large-scale plasmas leaves only virtual testing as a means to understand the universe. Advances in in computer technology and the capability of performing physics first principles, fully three-dimensional, particle-in-cell simulations, are making virtual testing a viable alternative to verify our predictions about the far universe.The first part of this paper explores the dynamical and fluid properties of the plasma state, plasma kinetics, and the radiation emitted from plasmas. The second part of this paper outlines the formulation for the particle-in-cell simulation of astrophysical plasmas and advances in simulational techniques and algorithms, as-well-as the advances that may be expected as the computational resource grows to petaflop speed/memory capabilities.Dedicated to the memories of Hannes Alfvén and Oscar Buneman; Founders of the Subject. 相似文献
19.
《Planetary and Space Science》2007,55(4):467-474
A theoretical study is made on the generation mechanism of electrostatic Bernstein mode wave in the presence of electromagnetic Kinetic Alfven wave turbulence in magnetized inhomogeneous plasma on the basis of plasma-maser interaction. It is shown that a test high-frequency electrostatic Bernstein mode wave is unstable in the presence of low-frequency Kinetic Alfven wave turbulence. Because of the universal existence of the Kinetic Alfven waves in large-scale plasmas, the result has potential importance in space and astrophysical radiation process. The growth rate of the test high-frequency Bernstein mode wave is obtained with the involvement of spatial density gradient parameter. A comparative study on the role of density gradient in the generation of Bernstein mode on the basis of plasma-maser effect is presented. 相似文献
20.
本文认为强磁场中的逆Compton散射可能是γ射线爆的主要辐射机制.其能谱是由源区质子产生的低频光子经强磁场中非热电子的Compton散射形成的.我们利用非相对论情形(B/B_(cr)≤1,hv_i/m_ec~2≤1)下强磁场中的Compton散射微分截面,导出了上述Compton散射的辐射谱公式,由此很好地拟合了典型γ射线爆GB811016的观测能谱. 相似文献