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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:20240328T110652Z
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
\nprovided the first firm proof that neutron star
mergers produce heavy
\nelements. Still\, it is not known exactly
which elements are produced by
\nmergers and in what proportions.
A full understanding of neutron star
\nmergers and their role in g
alactic chemical evolution requires progress in
\na number of area
s. Two key areas are neutrino and nuclear physics.
\nNeutrino phys
ics shapes the initial conditions for element synthesis\, and
\nth
e nuclear physics of extreme neutron-rich nuclei governs how the
\
nnucleosynthesis proceeds. Here we will review these microphysics aspe
cts
\nof neutron star merger nucleosynthesis and discuss how curre
nt
\nuncertainties influence our interpretations of observed abund
ance patterns
\nand kilonova signals. We will then explore the pro
mise of experimental
\ncampaigns at rare isotope beam facilities t
o both reduce these
\nuncertainties and provide insight into astro
physical environments of heavy
\nelement production.
URL:https://www.physics.wisc.edu/events/?id=4691
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