Dr
Ian Roederer
(Carnegie Observatories)
04/08/2012, 10:45
We present new abundance determinations of the heavy elements germanium (Ge, Z=32), arsenic (As, Z=33), selenium (Se, Z=34), and tellurium (Te, Z=52) in several metal-poor stars enriched with r-process material. These recent results mark the first detection of As, Se, and Te in an r-process environment beyond the solar system. In addition, detection of the elements at the third r-process...
Dr
Camilla Juul Hansen
(University of Heidelberg, ZAH)
04/08/2012, 11:15
The applications of stellar elemental abundances are numerous. The different groups of elements work as tracers of various formation processes, e.g. alpha-elements and odd-Z elements are created both in hydrostatic burning and supernova explosions. An abundances of every single element can trace differing features/parameters of the supernova such as mass and explosion energy.
By comparing...
Dr
Richard Cyburt
(JINA/MSU)
04/08/2012, 11:45
A reoccurring theme throughout nuclear astrophysics is the need for and use of the best available nuclear data as input for astrophysics calculations. Relevant nuclear data includes, but is not limited to nuclear masses, partition functions, thermonuclear reaction rates, weak interaction rates and fission fragment distributions. With the r-process reaction flow typically far from direct...
Dr
Kei Kotake
(National Astronomical Observatory of Japan)
04/08/2012, 13:30
In this contribution, we give overview about a current status
of multidimensional radiation hydrodynamic simulations of core-collapse supernovae. In addition to 3D hydrodynamics and general relativity, both of
which are now considered as the most important ingredients for making successful explosions, we discuss also impacts of nuclear equations of state on
the supernova dynamics. We...
Dr
Nobuya Nishimura
(University of Basel)
04/08/2012, 14:00
The problem of astrophysical site(s) for the r-process is still shrouded in mystery despite more than a half century of studies. Although neutrino driven winds have been considered to be the most likely success, recent state of the art hydrodynamic simulations show that it is seriously difficult to achieve suitable conditions for $r$-process by that scenario. We are reinvestigating the other...
Prof.
Bradley Meyer
(Clemson University)
04/08/2012, 14:30
The classical (n,gamma)-(gamma,n) phase of r-process nucleosynthesis is well understood. Less well understood is the complex freezeout phase during which the last of the free neutrons are consumed. I present some calculations using simplified nuclear physics to help characterize the r-process freezeout.
Almudena Arcones
(TU Darmstadt, GSI)
04/08/2012, 15:30
I will discuss the origin of lighter heavy elements (Sr, Y, Zr) in neutrino-driven winds.
Dr
Matthew Mumpower
(North Carolina State University)
04/08/2012, 16:00
The potential of an astrophysical environment for making r-process elements has been typically characterized by the neutron-to-seed ratio. We consider the rare earth peak as a new and independent tool for understanding the astrophysical conditions favorable for the main r-process. In the context of a high entropy r-process we discuss rare earth peak formation. We use features of a successful...
Dr
Shi-Sheng Zhang
(School of Physics and Nuclear Energy Engineering, Beihang University, Beijing 100191, China)
04/08/2012, 16:30
Single-particle resonant states embedded in the continuum for $^{131,133}$Sn, in the vicinity of the neutron capture threshold for $^{130,132}$Sn(n,$\gamma$), are calculated by the analytical continuation of the coupling constant (ACCC) approach within the relativistic mean field (RMF) theory framework. Our fully self-consistent RMF calculations using the NL3 effective interaction,
predict...
Prof.
Toshio Suzuki
(Nihon University)
04/08/2012, 17:00
β decays of the isotones with N = 126 are studied by shell-model calculations taking into account both the Gamow-Teller (GT) and first-forbidden (FF) transitions [1]. Shell-model interaction of Ref. [2] is adopted and a quenching of g_A^{eff}/g_A =0.7 is used for both the GT and FF transitions except for 0^{-} case. The FF transitions [3] are found to be important to reduce the beta-decay...
Prof.
Friedrich Thielemann
(University of Basel)
05/08/2012, 09:00
We give a short review on necessary conditions in order to achieve a sufficient neutron/seed ratio for an r-process to occur, what are the candidate astrophysical sites to fulfill such conditions (supernovae, magnetar-forming supernovae, quark (super-)novae, neutron star mergers,...), what is their role in the chemical evolution of galaxies, and whether there existed a chance to produce...
Prof.
Ani Aprahamian
(University of Notre Dame)
05/08/2012, 09:30
The rapid neutron capture process (r-process) is thought to be responsible for the creation of more than half of all elements beyond iron. The scientific challenges to understanding the origin of the heavy elements beyond iron lie in both the uncertainties associated with astrophysical conditions that are needed to allow an r-process to occur and a vast lack of knowledge about the properties...
Dr
Yuri Litvinov
(GSI, Darmstadt)
05/08/2012, 10:00
Ground state masses belong to the most essential nuclear quantities for our understanding of nucleosynthesis processes in stars. Particularly for the r-process, masses of very neutron-rich nuclei are needed. The need is best explained by the fact that mass differences of specific neighboring nuclei define the neutron separation energy and thus determine the pathway of the process on the chart...
Dr
Miguel Madurga
(University of Tennessee)
05/08/2012, 10:30
The $\beta$-decays of r-process neutron rich nuclei near the doubly magic
$^{78}$Ni were studied at the Holifield Radioactive Ion Beam
Facility (HRIBF) using an electromagnetic isobar
separator. The half-lives of $^{82}$Zn (228$\pm$10 ms),
$^{83}$Zn (117$\pm$20 ms) and $^{85}$Ga (93$\pm$7 ms) were
determined for the first time. These half-lives were found to be
dramatically different...
Jorge Pereira
(National Superconducting Cyclotron Laboratory and Michigan State University)
05/08/2012, 11:30
Despite more than half a century of intensive research, the nucleosynthesis of heavy nuclei remains is still an open questions in nuclear astrophysics. Besides the unknown scenario where the rapid neutron-capture process occurs, new incognita about the very synthesis mechanism are presently under study. The Puzzle will only be solved when the properties of the neutron-rich nuclei involved are...
Mr
Roger Caballero-Folch
(Universitat Politècnica de Catalunya (UPC))
05/08/2012, 12:00
β delayed neutron emission measurements around the third r-process peak
