5 edition of Turbulence, Waves and Instabilities in the Solar Plasma (NATO Science Series II: Mathematics, Physics and Chemistry) found in the catalog.
December 31, 2003 by Springer .
Written in English
|Contributions||R. Erdélyi (Editor), K. Petrovay (Editor), B. Roberts (Editor), Markus J. Aschwanden (Editor)|
|The Physical Object|
|Number of Pages||404|
Such anisotropies are consistent with the predictions of electron magnetohydrodynamics EMHD models, from both analytic theory [ 32 ] and computations [ 33 ]. Figure 1 shows the resulting reduced magnetic fluctuation spectra obtained by summing over one of the two perpendicular wavevector components. During the third phase, t 0. The long-wavelength kink mode and short-wavelength ballooning mode limits are generally well understood and can in principle be avoided. Chang et al.
Near observed frequencies of about 0. Using this Guide: Links to select e-books can be found by clicking on the tab associated with a particular subject. A well-known example of this is the pinch effect observed in specially designed equipment. February Plasmas in stars can both generate and interact with magnetic fieldsresulting in a variety of dynamic astrophysical phenomena. The shock wave travels toward the Sun at the same speed but in the opposite direction as the solar wind, so it appears to stand still with respect to the Earth.
These natural waves were used to probe the region of space around the Earth before spacecraft became available. Understanding of MHD stability gained in one configuration can benefit others, by verifying analytic theories, providing benchmarks for predictive MHD stability codes, and advancing the development of active control techniques. Whistler turbulence and whistler anisotropy instabilities a Whistler turbulence simulations The several PIC computational studies of whistler turbulence have assumed a homogeneous, collisionless, magnetized plasma on which an initial ensemble of relatively long-wavelength fluctuations are imposed; the individual modes satisfy the predictions of kinetic linear theory for whistler fluctuations. This good agreement provides confidence in ideal stability calculations for other configurations and in the design of prototype fusion reactors.
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In my opinion, definitive PIC simulations of possible interactions between cascading turbulence and enhanced instability-driven fluctuations have not yet been carried out. Between t 0. This result is consistent with the spectral transfer being due to nonlinear three-wave interactions which satisfy equation 1.
Numerical solution of the model in the linear regime demonstrates the capacity of the model to capture the salient characteristics of the two instabilities.
Nonlinear simulations of the unified model of the equatorial electrojet instabilities reproduce many of the features that are found in radar observations and sounding rocket measurements under multiple solar and ionospheric conditions. Note that the perpendicular heating rate is a nonnegligible fraction of that observed in the solar wind, where Hellinger et al.
In this case, the string represents a magnetic field line. Their results have been published and featured on the cover of Applied Physics Letters. The trip is so long that some waves those at higher frequencies arrive first, resulting in the generation of a whistlelike sound.
Among the various types of simulations used to study collisionless plasmas, PIC simulations provide the most general representation of plasma dynamics, but also require the greatest computational resources in terms of capacity and run times.
An equilibrium condition is reached in which the temperature is proportional to the square of the electric current. The linear and nonlinear numerical results of the 2-D unified fluid model are found to be comparable to the fully kinetic and hybrid models which have high computational cost and small coverage area of the ionosphere.
This is in agreement with the theoretical expectations, while the oblique firehose is unstable for moderately oblique wavevectors with respect to the magnetic field near the threshold; farther away from the threshold, the unstable modes become more oblique see Figure 3and these oblique angles are locally available between vortices where we observe the enhanced level of magnetic fluctuations.
Perpendicular to the magnetic field a different type of longitudinal wave called a magnetosonic wave can occur. These geometrical factors may be responsible for the late appearance of the instability but constraints on the instability timescales imposed by the turbulent nonlinearities are likely also important.
An oscillator can create an electrodeless discharge in gas at low pressure within a glass tube. In a recent studyscientists have revealed the cause of turbulence in the plasma, paving the way for the consistent application of this approach in the clinic.
Zoom Out Reset image size Figure 2. Even without particle collisions, waves shorter than the Debye length are heavily damped—i.
Note that our definition of turbulence includes all broadband fluctuations, whether they arrive at the short-wavelength regime by the classic forward cascade of multi-wave interactions or by other more general nonlinear processes such as those which act in the particle-in-cell PIC simulations of Karimabadi et al.
Resistive instabilities[ edit ] Resistive instabilities are an issue for all magnetic configurations, since the onset can occur at beta values well below the ideal limit. The spheromak requires wall stabilization to avoid the low-m, n tilt and shift modes, and possibly bending modes.
You can help by adding to it. The general instability condition is obtained. Whistler turbulence and whistler anisotropy instabilities a Whistler turbulence simulations The several PIC computational studies of whistler turbulence have assumed a homogeneous, collisionless, magnetized plasma on which an initial ensemble of relatively long-wavelength fluctuations are imposed; the individual modes satisfy the predictions of kinetic linear theory for whistler fluctuations.
The long-wavelength kink mode and short-wavelength ballooning mode limits are generally well understood and can in principle be avoided. In many cases MHD stability represents the primary limitation on beta and thus on fusion power density. Information about the the Synthesis Digital Library platform.
Two fundamental types of wave motion can occur: longitudinallike a sound or ion acoustic wave, in which particle oscillation is in a direction parallel to the direction of wave propagation; and transverselike a surface water wavein which particle oscillation is in a plane perpendicular to the direction of wave propagation.Dec 01, · The expansion of the solar wind away from the Sun drives electron velocity distributions away from the thermal Maxwellian form, yielding distributions near 1 AU which typically can be characterized as consisting of three anisotropic components: a more dense, relatively cool core, a relatively tenuous, relatively warm halo and a similarly tenuous, warm strahl.
Each of these Author: S. P. Gary. Save 40% on books and eBooks in Engineering & Materials Science or in Social & Behavioral with chapters on: magnetic clouds - interplanetary clouds - the solar wind plasma and MHD turbulence - waves and instabilities - energetic particles in the inner solar system.
Show all. Table of contents (6 chapters) Table of contents (6 chapters. Wave Instabilities in Space Plasmas Proceedings of a Symposium Organized within the XIXth URSI General Assembly Held in Helsinki, Finland, July 31–August 8, Some of the most important plasma instabilities and the irregularities they produce in the Earth's ionosphere are analyzed and discussed.
These include collisional interchange instabilities associated with equatorial spread F, collisional drift waves in midlatitude sporadic E -layers, Farley-Buneman waves in the auroral electrojet, and thermal.
Atmosphere, an international, peer-reviewed Open Access journal. A heuristic model of the turbulent flow that is consistent with the observations is one in which the energy for the turbulence is derived from the differential motion of the streams in the solar-wind plasma.
Instabilities associated with the differential streaming produce long-wavelength A1fv~n waves.