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PRODID:UW-Madison-Physics-Events
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SEQUENCE:1
UID:UW-Physics-Event-9572
DTSTART:20260219T213000Z
DTEND:20260219T223000Z
DTSTAMP:20260405T100923Z
LAST-MODIFIED:20260202T160510Z
LOCATION:4421 Sterling Hall
SUMMARY:Cosmic rays in cosmological simulations - bridging scales\, As
 tronomy Colloquium\, Dr. Ludwig Boess\, University of Chicago
DESCRIPTION:Galaxy clusters and their role in the large-scale structur
 e of the Universe\, the cosmic web\, have been studied extensively thr
 ough observations and simulations. However\, many of the high-energy p
 rocess that happen in these structures still elude observations and po
 se significant challenges for simulations of large-scale structure for
 mation.
\nMost notably\, the accretion of matter onto the cosmic web a
 nd the collisions of galaxy clusters embedded in it dissipate a large 
 fraction of their gravitational energy in the form of shocks. 
\nThese
  shocks heat the intra-cluster medium to keV energies and can accelera
 te protons and electrons to relativistic velocities.
\nNon-thermal emi
 ssion from relativistic electrons gives insight into the strength and 
 morphology of intra-cluster magnetic fields\, as well as providing pow
 erful tracers of structure formation shocks.
\nGamma-ray emission caus
 ed by CR protons on the other hand still challenges current observatio
 ns and is therefore testing models of proton acceleration at intra-clu
 ster shocks.
\nLarge-scale simulations which include the effects of CR
 s have been difficult to achieve since the difference between the scal
 e where CRs interact with the thermal gas and the resolution of these 
 simulations spans more than 20 orders of magnitude.
\nCosmic ray accel
 eration at astrophysical shocks have been studied extensively with PIC
  and hybrid simulations. However\, most of these simulations are limit
 ed to 2D due to computational constraints.
\nIn this talk\, I will giv
 e an overview of how we work to improve the modeling of CRs in large-s
 cale simulations of cosmological structure formation.
\nI will introdu
 ce the spectral CR model we use to evolve CR populations on-the-fly in
  our simulations and its application to simulations of the local Unive
 rse and will give an outlook on improvements to the PIC code entity wh
 ich we plan to use for 3D PIC simulations of ICM shocks.
URL:https://www.physics.wisc.edu/events/?id=9572
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