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Title:
Stochastic proton heating by kinetic-Alfvén-wave turbulence in moderately high-beta plasmas
Authors:
Hoppock, Ian W.; Chandran, Benjamin D. G.; Klein, Kristopher G.; Mallet, Alfred; Verscharen, Daniel
Affiliation:
AA(Space Science Center, University of New Hampshire, Durham, NH, 03824, USA), AB(Space Science Center, University of New Hampshire, Durham, NH, 03824, USA), AC(Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, 85719, USA), AD(Space Science Center, University of New Hampshire, Durham, NH, 03824, USA), AE(Space Science Center, University of New Hampshire, Durham, NH, 03824, USA)
Publication:
Journal of Plasma Physics, Volume 84, Issue 6, article id. 905840615, 21 pp.
Publication Date:
12/2018
Origin:
CUP
Keywords:
astrophysical plasmas, plasma heating, space plasma physics
Abstract Copyright:
(c) 2018: © Cambridge University Press 2018 This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution, and reproduction in any medium, provided the original work is properly cited.
DOI:
10.1017/S0022377818001277
Bibliographic Code:
2018JPlPh..84f9015H

Abstract

Stochastic heating refers to an increase in the average magnetic moment of charged particles interacting with electromagnetic fluctuations whose frequencies are smaller than the particles' cyclotron frequencies. This type of heating arises when the amplitude of the gyroscale fluctuations exceeds a certain threshold, causing particle orbits in the plane perpendicular to the magnetic field to become stochastic rather than nearly periodic. We consider the stochastic heating of protons by Alfvén-wave (AW) and kinetic-Alfvén-wave (KAW) turbulence, which may make an important contribution to the heating of the solar wind. Using phenomenological arguments, we derive the stochastic-proton-heating rate in plasmas in which p~1-30, where p is the ratio of the proton pressure to the magnetic pressure. (We do not consider the p≳30 regime, in which KAWs at the proton gyroscale become non-propagating.) We test our formula for the stochastic-heating rate by numerically tracking test-particle protons interacting with a spectrum of randomly phased AWs and KAWs. Previous studies have demonstrated that at p≲1, particles are energized primarily by time variations in the electrostatic potential and thermal-proton gyro-orbits are stochasticized primarily by gyroscale fluctuations in the electrostatic potential. In contrast, at p≳1, particles are energized primarily by the solenoidal component of the electric field and thermal-proton gyro-orbits are stochasticized primarily by gyroscale fluctuations in the magnetic field.
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