Bulletin of the American Physical Society
2012 Fall Meeting of the APS Division of Nuclear Physics
Volume 57, Number 9
Wednesday–Saturday, October 24–27, 2012; Newport Beach, California
Session KA: Awards Session |
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Chair: Berndt Mueller, Duke University Room: Plaza I |
Friday, October 26, 2012 2:00PM - 2:36PM |
KA.00001: Division of Nuclear Physics Mentoring Award Talk: Progress in Mentoring of Young Scientists in Nuclear Physics Invited Speaker: Michael Thoennessen The future of nuclear physics depends on attracting and retaining bright students. Several initiatives have begun to address issues related to successful recruiting and retention on various levels. Examples for undergraduate students, graduate students, post-docs, and faculty include the Conference Experience for Undergraduates at DNP meetings, the APS/AAPT Conference on Graduate Education, the NSF requirement for a post-doctoral mentoring plan, and the AAPT/AAS/APS New Faculty Workshops, respectively. In addition to these organized efforts, each member of the community can and should contribute to portraying nuclear physics as the exciting field that it is. [Preview Abstract] |
Friday, October 26, 2012 2:36PM - 3:12PM |
KA.00002: Dissertation Award in Nuclear Physics: Nuclear Equation of State in Astrophysics: Effect of Nuclear Symmetry Energy Invited Speaker: Gang Shen The equation of state for neutron rich matter plays a central role in many areas of nuclear astrophysics. One of key unknowns is the nuclear symmetry energy and its density dependence, which defines how different the neutron rich matter is from symmetric nuclear matter. I will discuss in detail a framework to generate a set of complete nuclear equations of state at finite temperature with distinct nuclear symmetry energy for the study of core collapse supernova and binary neutron star mergers. I will illustrate that, iso-vector interactions which give rise to the nuclear symmetry energy alter the kinematics of charged current reactions for electron neutrino and anti-neutrino in proto-neutron star. The electron fraction in the neutrino driven wind can thus be influenced by the nuclear symmetry energy. I will also describe a connection between the nuclear symmetry energy and the convection in proto-neutron star: it may have observable signature in the supernova neutrino signal, which can be measured in large water detectors such as SuperK. [Preview Abstract] |
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