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SEQUENCE:0
UID:UW-Physics-Event-3682
DTSTART:20150410T170000Z
DTEND:20150410T180000Z
DTSTAMP:20260419T142404Z
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.<br>
\n<br>
\n(coffee and c
 ookies at 11:45)
URL:https://www.physics.wisc.edu/events/?id=3682
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