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VERSION:2.0
CALSCALE:GREGORIAN
PRODID:UW-Madison-Physics-Events
BEGIN:VEVENT
SEQUENCE:1
UID:UW-Physics-Event-4691
DTSTART:20180504T203000Z
DURATION:PT1H0M0S
DTSTAMP:20260418T224717Z
LAST-MODIFIED:20180416T163400Z
LOCATION:2241 Chamberlin Hall
SUMMARY:The microphysics of the GW170817 kilonova\, Physics Department
  Colloquium\, Rebecca Surman\, Notre Dame University
DESCRIPTION:The optical signal that accompanied the GW170817 gravitati
 onal wave event<br>
\nprovided the first firm proof that neutron star 
 mergers produce heavy<br>
\nelements. Still\, it is not known exactly 
 which elements are produced by<br>
\nmergers and in what proportions. 
 A full understanding of neutron star<br>
\nmergers and their role in g
 alactic chemical evolution requires progress in<br>
\na number of area
 s. Two key areas are neutrino and nuclear physics.<br>
\nNeutrino phys
 ics shapes the initial conditions for element synthesis\, and<br>
\nth
 e nuclear physics of extreme neutron-rich nuclei governs how the<br>
\
 nnucleosynthesis proceeds. Here we will review these microphysics aspe
 cts<br>
\nof neutron star merger nucleosynthesis and discuss how curre
 nt<br>
\nuncertainties influence our interpretations of observed abund
 ance patterns<br>
\nand kilonova signals. We will then explore the pro
 mise of experimental<br>
\ncampaigns at rare isotope beam facilities t
 o both reduce these<br>
\nuncertainties and provide insight into astro
 physical environments of heavy<br>
\nelement production.
URL:https://www.physics.wisc.edu/events/?id=4691
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