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VERSION:2.0
CALSCALE:GREGORIAN
PRODID:UW-Madison-Physics-Events
BEGIN:VEVENT
SEQUENCE:2
UID:UW-Physics-Event-4637
DTSTART:20171016T170000Z
DTEND:20171016T180000Z
DTSTAMP:20260419T003842Z
LAST-MODIFIED:20171009T171631Z
LOCATION:Chamberlin 2241
SUMMARY:Cosmic Ray Dynamics in Galaxies and Galaxy Clusters\, Plasma P
 hysics (Physics/ECE/NE 922) Seminar\, Dr. Joshua Wiener\, UW Madison
DESCRIPTION:Cosmic rays (CRs) make up an important piece of many types
  of astronomical objects. Though few in number\, they can collectively
  contain as much energy as the thermal gas in galaxies and galaxy clus
 ters. It is therefore important to correctly model the transport of CR
 s in bulk in order to more completely understand the general dynamics 
 of these systems. I will briefly describe a simple CR transport model 
 where the bulk flow of CRs is limited by the streaming instability. I 
 will then apply this model to a number of systems of different scales:
  in galaxy clusters\, CRs are responsible for synchrotron emission see
 n as giant radio haloes. In galaxies\, CRs may be effective drivers of
  massive outflows\, playing a role in stellar feedback and regulation 
 of star formation. On smaller scales\, a CR-driven wind which is incid
 ent upon a cold dense cloud may be subject to a peculiar bottleneck ef
 fect\, which may impart significant momentum to the cloud as well as t
 hicken its interface with the surrounding hot gas.
URL:https://www.physics.wisc.edu/events/?id=4637
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