218 research outputs found
NHDS: The New Hampshire Dispersion Relation Solver
NHDS is the New Hampshire Dispersion Relation Solver. This article describes
the numerics of the solver and its capabilities. The code is available for
download on https://github.com/danielver02/NHDS.Comment: 3 pages, 1 figur
Instabilities Driven by the Drift and Temperature Anisotropy of Alpha Particles in the Solar Wind
We investigate the conditions under which parallel-propagating
Alfv\'en/ion-cyclotron (A/IC) waves and fast-magnetosonic/whistler (FM/W) waves
are driven unstable by the differential flow and temperature anisotropy of
alpha particles in the solar wind. We focus on the limit in which , where is the
parallel alpha-particle thermal speed and is the Alfv\'en
speed. We derive analytic expressions for the instability thresholds of these
waves, which show, e.g., how the minimum unstable alpha-particle beam speed
depends upon , the degree of alpha-particle
temperature anisotropy, and the alpha-to-proton temperature ratio. We validate
our analytical results using numerical solutions to the full hot-plasma
dispersion relation. Consistent with previous work, we find that temperature
anisotropy allows A/IC waves and FM/W waves to become unstable at significantly
lower values of the alpha-particle beam speed than in the
isotropic-temperature case. Likewise, differential flow lowers the minimum
temperature anisotropy needed to excite A/IC or FM/W waves relative to the case
in which . We discuss the relevance of our results to alpha
particles in the solar wind near 1 AU.Comment: 13 pages, 13 figure
Magnetohydrodynamic Slow Mode with Drifting He: Implications for Coronal Seismology and the Solar Wind
The MHD slow mode wave has application to coronal seismology, MHD turbulence,
and the solar wind where it can be produced by parametric instabilities. We
consider analytically how a drifting ion species (e.g. He) affects the
linear slow mode wave in a mainly electron-proton plasma, with potential
consequences for the aforementioned applications. Our main conclusions are: 1.
For wavevectors highly oblique to the magnetic field, we find solutions that
are characterized by very small perturbations of total pressure. Thus, our
results may help to distinguish the MHD slow mode from kinetic Alfv\'en waves
and non-propagating pressure-balanced structures, which can also have very
small total pressure perturbations. 2. For small ion concentrations, there are
solutions that are similar to the usual slow mode in an electron-proton plasma,
and solutions that are dominated by the drifting ions, but for small drifts the
wave modes cannot be simply characterized. 3. Even with zero ion drift, the
standard dispersion relation for the highly oblique slow mode cannot be used
with the Alfv\'en speed computed using the summed proton and ion densities, and
with the sound speed computed from the summed pressures and densities of all
species. 4. The ions can drive a non-resonant instability under certain
circumstances. For low plasma beta, the threshold drift can be less than that
required to destabilize electromagnetic modes, but damping from the Landau
resonance can eliminate this instability altogether, unless .Comment: 35 pages, 5 figures, accepted for publication in Astrophys.
Stochastic relativistic shock-surfing acceleration
We study relativistic particles undergoing surfing acceleration at
perpendicular shocks. We assume that particles undergo diffusion in the
component of momentum perpendicular to the shock plane due to moderate
fluctuations in the shock electric and magnetic fields. We show that dN/dE, the
number of surfing-accelerated particles per unit energy, attains a power-law
form, dN/dE \propto E^{-b}. We calculate b analytically in the limit of weak
momentum diffusion, and use Monte Carlo test-particle calculations to evaluate
b in the weak, moderate, and strong momentum-diffusion limits.Comment: 20 pages, 6 figures, accepted by ApJ; this version corrects a few
minor typographical error
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