2005 47th Annual Meeting of the Division of Plasma Physics
Monday–Friday, October 24–28, 2005;
Denver, Colorado
Session KI2: Basic Plasma Physics II
9:30 AM–12:30 PM,
Wednesday, October 26, 2005
Adam's Mark Hotel
Room: Plaza Ballroom EF
Chair: Antonio Ting, Naval Research Laboratory
Abstract ID: BAPS.2005.DPP.KI2.1
Abstract: KI2.00001 : Turbulent Heating and Fluctuation Characteristics in Alfvenic Turbulence
9:30 AM–10:00 AM
Preview Abstract
Abstract
Author:
William Dorland
(Department of Physics, University of Maryland, College Park, MD, 20742)
Alfve\'n waves are ubiquitous in natural and laboratory plasmas.
In this talk, the
main focus is on astrophysical plasmas that are turbulent,
magnetized, hot and
diffuse. The dynamically important characteristics of these
plasmas are often well-
described by magnetohydrodynamics [see {\it e.g.,} Ref.~1].
However, much of what
we actually observe is critically affected by how much of the
turbulent energy is
absorbed by (highly radiative) electrons [2], the amplitude of
density fluctuations
[3], and the spectral indices of turbulent, Alfve\'nic cascades.
These questions each
have essentially kinetic aspects. In this talk, we present
detailed simulations and
analyses of of the cascade of shear Alfve\'n waves, to and
through scales
comparable to the ion Larmor radius in the direction
perpendicular to the magnetic
field. We demonstrate analytically and numerically that the
nonlinear gyrokinetic
equations, originally developed for fusion applications, are
perfectly suited to these
astrophysical problems. We present extensive linear and
nonlinear gyrokinetic
simulation results from the {\tt GS2} code. We demonstrate
accurate resolution of
the damping of kinetic Alfve\'n waves in plasmas with beta small,
large and
comparable to unity, for a wide range of electron-to-ion
temperature ratios, in
linear and nonlinear contexts. We have used the {\tt GS2} code
to calculate the
turbulent energy absorption, density fluctuation characteristics,
and spectral indices
for plasmas with parameters taken from hot accretion flows and
from the
interstellar plasma. These results will be compared with
theoretical predictions [2]
and to observations.
\noindent
Co-authors: S.~C.~Cowley (UCLA), G.~W.~Hammett (PPPL),
E.~Quataert and
G.~Howes (UC-Berkeley), and A.~Scheckochihin (Cambridge)
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1. S.~Balbus and J.~Hawley, Rev Mod Phys, Vol.~70, p.~1. \\
2. E.~Quataert and A.~Gruzinov, Ap J, Vol.~520, p.~248;
E.~Quataert, Ap J,
Vol.~500, p.~978.\\
3. Y.~Lithwick and P.~Goldreich, Ap J, Vol.~562, p.~279.\\
4. P.~Goldreich and Sridhar, Ap J, Vol.~438, p.~763; P.~Goldreich
and Sridhar, Ap J,
Vol.~485, p.~680.
To cite this abstract, use the following reference: http://meetings.aps.org/link/BAPS.2005.DPP.KI2.1