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SUMMARY:Modeling Cosmic Ray Acceleration by Galactic Wind Termination Shoc
 ks
DTSTART:20170509T200600Z
DTEND:20170509T202400Z
DTSTAMP:20260722T090100Z
UID:indico-contribution-5273@events.icecube.wisc.edu
DESCRIPTION:Speakers: Chad Bustard (University of Wisconsin - Madison)\, E
 llen Zweibel (UW-Madison)\, Cory Cotter (UW-Madison)\n\nDiffusive shock ac
 celeration (DSA) at supernova remnant (SNR) shock fronts is thought to acc
 elerate galactic cosmic rays (CRs) to energies below the knee\, while an e
 xtragalactic origin is presumed for CRs with energies beyond the ankle. CR
 s with energies between 3 × 1015 and 1018 eV\, which we dub the "shin\," 
 have an unknown origin. It has been proposed that DSA at galactic wind ter
 mination shocks\, rather than at SNR shocks\, may accelerate CRs to these 
 energies. Our work uses the galactic wind model of Bustard et al. (2016) t
 o analyze whether galactic wind termination shocks may accelerate CRs to s
 hin energies within a reasonable acceleration time and whether such CRs ca
 n subsequently diffuse back to the Galaxy\, where they can interact with d
 ense ambient material to produce gamma-rays and neutrinos. I will argue fo
 r acceleration times on the order of 100 million years rather than a few b
 illion years\, as assumed in some previous works\, and I will outline our 
 analytic formulae\, applicable to any wind model\, for CR acceleration. Ev
 en with generous assumptions\, we find that very high wind velocities are 
 required to set up the necessary conditions for acceleration beyond 1017 e
 V. We also estimate the luminosities of CRs accelerated by outflow termina
 tion shocks\, including estimates for the Milky Way wind.\n\nhttps://event
 s.icecube.wisc.edu/event/82/contributions/5273/
LOCATION:Forum (Discovery Building)
RELATED-TO:indico-event-82@events.icecube.wisc.edu
URL:https://events.icecube.wisc.edu/event/82/contributions/5273/
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