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UID:UW-Physics-Event-3682
DTSTART:20150410T170000Z
DTEND:20150410T180000Z
DTSTAMP:20240329T003706Z
LAST-MODIFIED:20150404T160943Z
LOCATION:2241 Chamberlin Hall - Coffee and cookies at 11:45
SUMMARY:Kinetic and Gyrokinetic Astrophysical Turbulence Above and Bel
ow the Mirror and Firehose Stability Thresholds\, Physics Department C
olloquium\, Matt Kunz\, Princeton
DESCRIPTION:The solar wind is weakly collisional. As such\, the partic
le populations that comprise it exhibit a variety of non-Maxwellian fe
atures\, which are customarily described in terms of interspecies drif
ts and pressure anisotropies relative to the magnetic field direction.
The solar wind is also turbulent\, with a power spectrum extending ov
er many orders of magnitude above and below the ion Larmor scale. Thes
e two facts\, both well documented by the observational community\, ar
e not always treated on equal footing in concomitant theoretical work.
Current gyrokinetic and reduced-MHD treatments of solar-wind turbulen
ce take the plasma distribution to be Maxwellian. Analyses of pressure
-anisotropy-driven Larmor-scale instabilities rarely focus on their co
ntribution to the kinetic-scale turbulent cascade. These issues borne
in mind\, I will present some analytical and numerical efforts to cons
truct a more suitable theoretical framework for describing inertial-ra
nge and Larmor-scale kinetic turbulence in non-Maxwellian astrophysica
l plasmas. Implications for turbulence in other weakly collisional env
ironments\, such as radiatively inefficient accretion flows and the in
tracluster medium\, will also be discussed.
\n
\n(coffee and c
ookies at 11:45)
URL:https://www.physics.wisc.edu/events/?id=3682
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