Program - Brookhaven National Laboratory

elow the neutron separation energy and determination of the spin and parity of neutron resonances. The
deformed rare earth region is particularly interesting for the study of the effects of nuclear deformation on
the isovector magnetic-dipole resonance, referred as the scissors mode (SM) resonance. The SM strength
is expected to be proportional to the square of the nuclear deformation parameter. The results of the
dysprosium experiments and some results on the data analysis will be presented.
Session LB Nuclear Astrophysics
Wednesday March 6, 2013
Room: Met West at 3:30 PM
LB 1 3:30 PM
The “Karlsruhe Astrophysical Database of Nucleosynthesis in Stars” project - Status and
Prospects
Iris Dillmann, Justus-Liebig-Universität Giessen and GSI Helmholtzzentrum für Schwerionenforschung,
Germany. Ralf Plag, GSI Helmholtzzentrum für Schwerionenforschung and Goethe-Universität Frankfurt,
Germany. Tamas Szücs and Zsolt Fülöp, Institute of Nuclear Research (ATOMKI), Debrecen/Hungary.
Thomas Rauscher, Universität Basel/ Switzerland. Franz Käppeler, KIT Karlsruhe Institute of
Technology, Campus Nord, Karlsruhe/ Germany.
The nuclei heavier than iron are produced mainly by the “slow” and the “rapid neutron capture process,”
and a third subset of processes which is responsible for up to 35 stable proton-rich “p nuclei.” The first two
involve neutron capture reactions and β-decays, whereas the main reaction mechanism for the “p nuclei” is
the “gamma process” which requires also proton- and alpha-induced reactions within the Gamow window
of T=2-3 billion Kelvin. The “Karlsruhe Astrophysical Database of Nucleosynthesis in Stars” (KADoNiS)
project is an online database for experimental cross sections relevant to the s-process and p-process. It
is available under http://www.kadonis.org and consists of two parts. Part 1 is an updated sequel to the
previous Bao et al. compilation for stellar (n,gamma) cross sections relevant to nucleosynthesis in the Big
Bang and in the s-process [1]. This database was launched in 2005 and is updated every 2 years [2,3]. Until
now, recommended Maxwellian averaged cross sections (MACS) at stellar temperatures between kT=5 and
100 keV are given for more than 350 isotopes on the s-process reaction path. After the last full update in
2011 the database was further extended into the neutron-rich region taking into account the requirements
of modern stellar s-process models, and by inclusion of (n,p) reactions of light isotopes. The second part of
the KADoNiS project is a collection of all available experimental cross sections in or close to the respective
Gamow window for the “gamma process” and the comparison with various theoretical models. In 2006 a
first trial within the KADoNiS project was launched, but it lasted until 2010 until this part was improved
in collaboration with the ATOMKI Debrecen and the updated p-process database was published [4,5].
We will give an overview about the KADoNiS project and present the status and improvements of the
s-process database which is just about to be published. I.D. is supported by the Helmholtz association
via the Young Investigators project VH-NG-627. R.P. is supported by the Helmholtz association via the
Young Investigators project VH-NG-327. T.Sz. is supported by EUROGENESIS OTKA-NN83261. Zs.F.
is supported by OTKA K68809.
[1] Z.Y. Bao et al., At. Data Nucl. Data Tables 76 (2000) 70. [2] I. Dillmann, M. Heil, F. Käppeler, R.
Plag, T. Rauscher, and F.-K. Thielemann, AIP Conf. Proc. 819, 123 (2006). [3] I. Dillmann, R. Plag, F.
Käppeler, T. Rauscher, Proc. “EFNUDAT Fast Neutrons - scientific workshop on neutron measurements,
theory & applications,” April 28-30 2009, Geel, Belgium, p.55. [4] T. Szücs, I. Dillmann, R. Plag, and Zs.
Fülöp, Proceedings of Science (2011), PoS(NIC XI)247 [5] T. Szücs, I. Dillmann, R. Plag, and Zs. Fülöp,
J. Phys.: Conf. Ser. 337, 012033 (2012).
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