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ISNAP Seminars - Abstracts 2015 Fall


Topic: ANCs at sub-Coulomb energies to constrain key α-capture reaction rates

Dr. Melina Avila ( Argonne National Laboratory ) / August 24, 2015

Many important α-particle induced reactions can only be measured indirectly due to small cross section at energies of astrophysical interest. Extracting the Asymptotic Normalization Coefficients (ANCs) using sub-Coulomb α-transfer reactions can be used as an effective method to determine properties of near-threshold resonances. This will constrain and drastically limit the uncertainties related to extrapolations procedures for key astrophysical reactions. We have applied this valuable tool to investigate the important α-capture reactions 12C(α, γ)16O and 13C(α, n)16O. Results and the implication to the astrophysical rates will be discussed.


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Dr. Antonio Villari ( NSCL / MSU ) / September 28, 2015



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Mr. Sean Kuvin ( Florida State University ) / October 5, 2015



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Prof. Sandrine Courtin ( Institut Pluridisciplinaire Hubert Curien, Strasbourg, France ) / October 12, 2015



Topic: Discovery of Supernova-produced 60Fe in the Earth's Fossil Record

Dr. Shawn Bishop ( Technical University of Munich, Germany ) / October 19, 2015

Approximately 1.8 to 2.8 Myr before the present our planet was subjected to the debris of a supernova explosion. The terrestrial proxy for this event was the discovery of live atoms of 60Fe in a deep-sea ferromanganese crust [1]. The signature of this supernova event should also reside in magnetite (Fe3O4) magnetofossils produced by magnetotactic bacteria [2], which live in the ocean sediments, extant at the time of the Earth-supernova interaction. We have conducted accelerator mass spectrometry (AMS) measurements, searching for live 60Fe atoms in the magnetofossil component of Pacific Ocean sediment cores (ODP cores 848 and 851). We find a time-resolved 60Fe signal in both sediment cores, above background, centered at approximately 2 Myr ago and spanning approximately 700 kyr duration (full width half maximum), which will require eventual astrophysical interpretation to understand.
The production of elements beyond Fe occurs partly in what is known as the "r-process". This process involves the rapid capture of neutrons on time scales of milliseconds, temperatures of GK and densities of 109 g/cm3. The global physics of how the r-process works is largely understood; what is not known, however, is where in the universe it occurs. Candidate sites for the r-process are core collapse supernovae or binary neutron star mergers. The former is theoretically and observationally known to produce 60Fe; the latter is theoretically expected to produce negligible amounts of 60Fe. The heavy actinides, for example, are themselves r-process "only" nuclides; that is, they can only be made through the r-process. Present theoretical models favour r-process production in neutron star mergers over core collapse supernovae. Therefore, any future finding of a short-lived r-process "only" isotope in terrestrial reservoirs, coincident in time with the observed 60Fe signal, would show that core collapse supernovae are at least one site, in our cosmos, in which the r-process occurs.
This talk is designed to be accessible to a broad audience.
[1] Knie et al., Phys. Rev. Lett. 93, 171103 (2004).
[2] S. Bishop and R. Egli, Icarus 212, 960 (2011).


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Prof. Bradley Meyer ( Clemson University ) / November 9, 2015



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Dr. Kyle Leach ( TRIUMF, Canada ) / November 16, 2015



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Dr. Farheen Naqvi ( NSCL / MSU ) / November 23, 2015



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