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VERSION:2.0
CALSCALE:GREGORIAN
PRODID:UW-Madison-Physics-Events
BEGIN:VEVENT
SEQUENCE:1
UID:UW-Physics-Event-4950
DTSTART:20181126T180500Z
DURATION:PT1H0M0S
DTSTAMP:20260419T060555Z
LAST-MODIFIED:20181113T184233Z
LOCATION:2241 chamberlin hall
SUMMARY:Turbulent Dynamo in a Collisionless Magnetized Plasma\, Plasma
  Physics (Physics/ECE/NE 922) Seminar\, Denis St-Onge\, Princeton Univ
 .
DESCRIPTION:The Universe is magnetized. While magnetic-field strengths
  of just ~10-18 G are required to achieve this both in our Galaxy and 
 in clusters of galaxies\, observations of Faraday rotation\, Zeeman sp
 litting\, and synchrotron emission all make the case of ubiquitous mic
 rogauss fields. That these systems are not content with hosting weaker
  fields is surprising\, at least until one realizes that the energy de
 nsity of a microgauss field is comparable to that of the observed turb
 ulent motions. It is then natural to attribute the amplification and s
 ustenance of (at least the random component of) the interstellar and i
 ntracluster magnetic fields to the fluctuation (or “turbulent”) dy
 namo. In this talk\, we will explore the various ways in which plasma 
 microphysics makes magnetic-field amplification in weakly collisional 
 plasmas by macroscale turbulent motions possible\, with application to
  the intracluster medium of galaxy clusters.
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URL:https://www.physics.wisc.edu/events/?id=4950
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