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Upcoming Seminars & Lectures

DateTime SpeakerLocationTitle  (click on title to see abstract)
Today,
2018-02-21
14:30AcceleratorValery Radchenko
TRIUMF
ISAC II Conf RmProduction of medical radionuclides at TRIUMF: current status and future perspectives.
Thu ,
2018-02-22
14:00ColloquiumThomas Planche
TRIUMF
AuditoriumThe Cow is not Spherical: Space Charge in TRIUMF Accelerators.
Fri ,
2018-02-23
14:30SpecialPSD Mixer
TRIUMF
AuditoriumPhysical Sciences Division Mixer
Wed ,
2018-02-28
11:00AcceleratorDoug Storey
University of Victoria / TRIUMF
ISAC II Conf RmThe Superconducting RF Deflecting Cavity for the ARIEL e-Linac Separator
Wed ,
2018-02-28
16:00SpecialNick Zacchia
TRIUMF/ UBC
MOB BoardroomIsoSiM Seminar: Report IRE stay in Germany
Thu ,
2018-03-01
14:00ColloquiumGaute Hagen
Oak Ridge National Laboratory
AuditoriumA solution to the puzzle of quenched beta-decays and a quantum computation of an atomic nucleus
Thu ,
2018-03-08
14:00ColloquiumCharles Horowitz
University of Indiana
AuditoriumThe neutron star merger GW170817 and neutron rich matter in the laboratory and in the heavens
Abstract:Compress almost anything to very high densities and electrons react with protons to make neutron rich matter. This material is at the heart of many fundamental questions in nuclear physics and astrophysics. What are the high-density phases of QCD? Where did the chemical elements come from? What is the structure of many compact and energetic objects in the heavens, and what determines their electromagnetic, neutrino, and gravitational-wave radiations? Recently, extensive gravitational wave and electromagnetic observations of the neutron star merger GW170817 have constrained the equation of state of neutron rich matter and strongly suggest that neutron star mergers are an important site of rapid neutron capture (r-process) nucleosynthesis of heavy elements such as gold and uranium. We discuss these historic developments and try and place them in a broad context. We describe how the thickness of the neutron skins of the 48Ca and 208Pb nuclei are being measured with parity violating electron scattering at Jefferson Laboratory. These skins depend on the pressure of neutron rich matter and have important implications for the structure of neutron stars. We expect many thousand neutrino events from the next galactic core collapse supernova (SN). Simple neutrino interactions suggest that the neutrino driven wind is not very neutron rich and thus, despite what is said in many textbooks, SN may not be the site of the r-process for heavy elements. Finally, GW170817, by suggesting the astrophysical conditions, has set the stage for TRIUMF ISAC / ARIEL and other radioactive beam facilities to perform detailed studies of r-process nucleosynthesis.
 
Wed ,
2018-03-14
16:00SpecialYang Lan
TRIUMF/ UBC
AuditoriumIsoSiM Seminar: Report IRE stay in Germany
Thu ,
2018-03-22
14:00ColloquiumBrad Filippone
Caltech
AuditoriumTBA
Wed ,
2018-03-28
16:00SpecialVesna Sossi
UBC
AuditoriumIsoSiM Seminar: tba
Thu ,
2018-03-29
14:00ColloquiumRoger Melko
U Waterloo
AuditoriumMachine Learning the Many-Body Problem
Thu ,
2018-04-05
14:00ColloquiumJoseph Bramante
CPARC/Queen's U
AuditoriumUsing Neutron Star Mergers to Search for Asymmetric Dark Matter
Mon ,
2018-05-07
14:00SpecialPaul Lecoq
CERN
AuditoriumThe 10ps TOFPET Challenge, Myth or Reality