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DICTIONARY OF GEOPHYSICS, ASTROPHYSICS, and ASTRONOMY

DICTIONARY OF GEOPHYSICS, ASTROPHYSICS, and ASTRONOMY

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static equilibrium, air parcels have zero vertical<br />

acceleration. There is no absolutely zero vertical<br />

acceleration in real atmosphere, especially in<br />

small scale weather systems. However, for large<br />

scale weather systems, comparing to the gravitational<br />

acceleration, the vertical acceleration is<br />

very small <strong>and</strong> can be neglected, <strong>and</strong> thus the<br />

quasi-hydrostatic approximation is appropriate.<br />

quasi-linear theory In plasma physics, a theory<br />

based on perturbation theory; interactions<br />

between waves <strong>and</strong> particles are considered to<br />

be first order only. As in perturbation theory, all<br />

terms of second order in the fluctuating quantities<br />

should be small enough to be ignored. Only<br />

weakly turbulent wave-particle interactions can<br />

be treated this way: The particle distribution is<br />

only weakly affected by the self-excited waves<br />

in a r<strong>and</strong>om-phase uncorrelated way. This requirement<br />

not only corresponds to small disturbances<br />

in perturbation theory but even directly<br />

results from it as the waves are described in the<br />

framework of perturbation theory. The waves<br />

generatedbytheparticleswillaffecttheparticles<br />

inawaythatwilltendtoreducethewaves. Thus,<br />

the plasma is assumed to be a self-stabilizing<br />

system: Neither indefinite wave growth happens<br />

nor can the particles be trapped in a wave well.<br />

The basic equation of quasi-linear theory is<br />

the Vlasov equation. All quantities then are split<br />

into a slowly evolving part <strong>and</strong> a fluctuating part.<br />

The long-term averages of the fluctuating part<br />

vanish. In quasi-linear theory, the slowly evolving<br />

quantities give the evolution of the system<br />

under study, while in case of the plasma waves<br />

the fluctuating quantities are of interest because<br />

they describe the wave.<br />

With the index ‘o’ describing the slowly<br />

evolving quantities <strong>and</strong> the index ‘1’ giving the<br />

fluctuating quantities, the average Vlasov equation<br />

as the basic equation of quasi-linear theory<br />

can be written as<br />

∂fo<br />

+<br />

∂t+ v ·∇fo<br />

q v × Bo<br />

·<br />

m c<br />

∂fo<br />

∂v<br />

=− q<br />

<br />

<br />

v × B1<br />

E1 + ·<br />

m<br />

c<br />

∂f1<br />

<br />

.<br />

∂v<br />

with f being the phase space density, v the<br />

plasma speed, q the charge, m the mass of the<br />

charged particles, E the electric, <strong>and</strong> B the magnetic<br />

field. The term on the right-h<strong>and</strong> side con-<br />

© 2001 by CRC Press LLC<br />

quasi-viscous force<br />

tains the non-vanishing averages of the fluctuations<br />

<strong>and</strong> describes the interaction between the<br />

fluctuating fields <strong>and</strong> the fluctuating part of the<br />

particle distribution. These interactions, combined<br />

with the slowly evolving fields on the lefth<strong>and</strong><br />

side lead to the evolution of the slowly<br />

evolving part of the phase space density. Note<br />

that no assumption about the smallness of the<br />

fluctuations enters: The only limitation is a clear<br />

separation between the fluctuating part <strong>and</strong> the<br />

average behavior of the plasma. See perturbation<br />

theory.<br />

quasi-neutral equilibrium A plasma condition<br />

apparently occurring on magnetic field lines<br />

in the auroral oval, in which a parallel electric<br />

field is balanced by the mirror force on precipitating<br />

electrons. The parallel voltage may originate<br />

in the circuit that powers Birkel<strong>and</strong> currents<br />

linking the auroral ionosphere with the distant<br />

magnetosphere. It accelerates the auroral electrons<br />

<strong>and</strong> at the same time exp<strong>and</strong>s the loss cone,<br />

allowing an increase in the current intensity.<br />

quasi-separatrix layer Generalizations of<br />

magnetic separatrices to magnetic configurations<br />

with a non-zero magnetic field strength<br />

everywhere in a given region. They are the locations<br />

where drastic changes in field-line linkages<br />

occur in the solar atmosphere.<br />

quasi-single-scattering approximation A<br />

radiative transfer model that accounts for only<br />

single scattering of photons with the assumption<br />

that forward-scattered light is treated as unscattered.<br />

quasi stellar object See QSO.<br />

quasi-viscous force A force transferring momentum<br />

through the magnetopause, from the solar<br />

wind flowing past Earth to the plasma inside<br />

the geomagnetic tail. A quasi-viscous force was<br />

proposed in 1961 by Ian Axford <strong>and</strong> Colin Hines<br />

as a possible mechanism for causing global convection<br />

in the Earth’s magnetosphere. Magnetic<br />

reconnection, proposed the same year by James<br />

Dungey, is an alternative mechanism, <strong>and</strong> many<br />

researchers believe both mechanisms are active,<br />

with the quasi-viscous force being the weaker<br />

but steadier factor.<br />

383

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