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SUMMARY:Cosmic rays in star-forming galaxies - Mark Krumholz (ANU)
DTSTART:20240906T103000Z
DTEND:20240906T113000Z
UID:TALK216907@talks.cam.ac.uk
CONTACT:Sandro Tacchella
DESCRIPTION:Supernovae ultimately deposit ~10% of their total energy in a 
 population of relativistic cosmic rays. Because these particles lose energ
 y to radiation only slowly compared to the ~90% of the supernova energy th
 at is deposited in the interstellar medium as heat\, they are a potentiall
 y important feedback mechanism in galaxies despite their comparatively sma
 ll energy budget. Their effectiveness\, however\, depends crucially on the
  poorly-understood plasma processes that couple them to the background gas
 \, which spans a huge range of properties from cool and mostly-neutral ato
 mic and molecular gas to hot ionised medium\, with most of the mass over m
 ost of cosmic time residing in the former phase. We lack a complete theory
  for cosmic ray-gas coupling in part due to the paucity of observational c
 onstraints on cosmic ray transport\, which are limited beyond the Solar ne
 ighbourhood\, and even scarcer for extragalactic systems. In this talk I d
 iscuss recent progress towards connecting microphysical models for cosmic 
 ray transport to observable predictions for CR-driven non-thermal emission
 \, and the implications of these results for theories of cosmic ray transp
 ort. I conclude by exploring some of the new frontiers in this area that w
 ill be opened by the advent of the CTA and\, later in the decade\, the SKA
 .\n
LOCATION:Ryle seminar room + online
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