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VERSION:2.0
CALSCALE:GREGORIAN
PRODID:UW-Madison-Physics-Events
BEGIN:VEVENT
SEQUENCE:0
UID:UW-Physics-Event-2865
DTSTART:20121206T213000Z
DTEND:20121206T230000Z
DTSTAMP:20260412T060715Z
LAST-MODIFIED:20121128T171623Z
LOCATION:4421 Sterling Hall
SUMMARY:Adaptive Mesh Refinement Dimulations of Cosmic Rays in Cluster
 s of Galaxies\, Astronomy Colloquium\, Samuel Skillman\, University of
  Colorado
DESCRIPTION:The observed properties of galaxy clusters are the result 
 of a non-linear interaction between many physical processes including 
 gravity\, hydrodynamics\, magnetic fields\, turbulence\, radiation\, g
 alaxy formation and feedback\, and cosmology. This provides a unique "
 cosmic laboratory" with which we can learn about our Universe.  In par
 ticular\, galaxy clusters are hosts to cosmic shocks\, which propagate
  through the intracluster medium as a signature of structure formation
 . It is believed that at these shock fronts\, magnetic field inhomogen
 eities in a compressing flow may lead to the acceleration of cosmic ra
 y electrons and ions. These relativistic particles decay and radiate t
 hrough a variety of mechanisms\, and have observational signatures in 
 radio\, hard X-ray\, and Gamma-ray wavelengths. The construction of se
 veral new low frequency radio telescopes have begun observations of aE
 urooeradio relicsaEuro\, which are thought to be the result of synchro
 tron emission from shock accelerated electrons.  I will present recent
  work using adaptive mesh refinement MHD simulations of galaxy cluster
 s using Enzo and analyzed with yt\, that explain many of the observed 
 properties of these radio relics including polarization fraction and d
 irection of the radiation.  I will also present preliminary work of co
 mbining a numerical library for momentum-space transport of cosmic ray
 s with Enzo\, where we can follow the spectral evolution of these high
  energy particles along with their spatial transport.
URL:https://www.physics.wisc.edu/events/?id=2865
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