10-11 September 2009
Max-Planck Institut fuer Extraterrestrische Physik (MPE)
Europe/Berlin timezone
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Displaying 16 contributions out of 16
Session: gamma-process II
E062 Collaboration
Presented by Michael HEIL on 10 Sep 2009 at 16:15
The gamma ray strength function of heavy nuclei is an important quantity to determine their reaction rates in in high temperature environments envisioned in explosive nucleosynthesis. Especially p-process nuclides are formed through sequences of photodisintegrations from sand r-process seeds. In these reactions the gamma ray strength function around the neutron separation energy on the low ene ... More
Presented by Arnd R. JUNGHANS on 11 Sep 2009 at 11:15
Session: gamma-process I
In order to extend the available experimental database of alpha-induced reactions relevant for the p-process towards the heavier mass region, the cross section of the 151Eu( alpha,gamma)155Tb and 151Eu(alpha,n)154Tb reactions has been measured using the activation technique. The cross sections have been detemined in the center-of-mass energy range of 11.2 – 17 MeV and 12.3 – 17 MeV for the (a ... More
Presented by Gyorgy GYURKY on 10 Sep 2009 at 14:00
Session: gamma-process I
The 146Sm nuclide (t1/2= 1.03x10^8 a) belongs to the small family of nuclides produced by the nucleosynthesis p-process . Its presence as live radionuclide in the Early-Solar System was established by the study of isotopic anomalies of its 142Nd alpha daughter in meteorites. Interestingly, a difference in 142Nd isotopic signatures has been also discovered between terrestrial and chondritic materi ... More
Presented by Michael PAUL on 10 Sep 2009 at 15:10
Session: rp-process
Type I X-ray bursts are thermonuclear runaways that occur on the surface of neutron stars in binary systems with low-mass companions. These systems, in some cases, host the so-called rapid proton capture process (rp–process) [1,2]. Under high temperature (T ~2 GK) and density (rho> 1E5 g/cm3) conditions in the burning layer, the nuclear reaction network of the rp- process runs close to the proto ... More
Presented by Daniel GALAVIZ on 11 Sep 2009 at 09:15
Session: rp-process
The masses of proton-rich nuclides in the element range from Sr to Tc were measured with the Penning trap mass spectrometer SHIPTRAP [1] at GSI. These nuclei were produced in the fusion-evaporation reaction 36Ar + 54Fe at energies of 5.0 and 5.9 MeV/u and separated by the velocity filter SHIP [2]. Their masses were measured with relative accuracies ranging from 5·10-8 to 2·10-7. The masses o ... More
Presented by Emma HAETTNER on 11 Sep 2009 at 10:05
Session: gamma-process II
Proton, neutron and alpha-particle capture reactions are the main contributors towards the understanding of the p-process nucleosynthesis. Although the reactions involved in this process are mainly photodisintegrations, measuring the inverse reactions can be even more helpful than the measurement of the gamma -induced reactions themselves. Recently there have been major experimental efforts ... More
Presented by Artemis SPYROU on 10 Sep 2009 at 15:45
Session: gamma-process II
The p-process is the most promising astrophysical scenario for the nucleosynthesis of about 35 proton-rich nuclei referred to as p nuclei. This process involves an extensive reaction network of about 2000 nuclei and more than 20000 reactions, especially photodisintegration reactions, under explosive physical conditions. The huge number of reaction rates are mainly adopted from Hauser-Feshbach ... More
Presented by Jens HASPER on 10 Sep 2009 at 16:45
Presented by Jens HASPER on 11 Sep 2009 at 10:45
Session: gamma-process I
ATOMKI has a long range program, supported by the European Research Council, to study reactions relevant to p-process using low energy accelerators. In addition to the alpha-induced reactions, proton-induced cross section data can test the reliability of the model calculations in the proton rich region as well as provide experimental information directly relevant to the p-process. Recent advan ... More
Presented by Zsolt FULOP on 10 Sep 2009 at 14:30
A short overview is given about ongoing activities concerning the p-process library in the Karlsruhe Astrophysical Database of Nucleosynthesis in Stars (www.kadonis.org). For this project a collaboration with the ATOMKI in Debrecen has been established.
Presented by Iris DILLMANN, Tamas SZUCS on 11 Sep 2009 at 12:30
Session: rp-process
A complete understanding of the synthesis of the elements is one of the main outstanding questions in nuclear astrophysics. A number of nucleosynthesis processes are known and to a reasonable extent account for much of the observed solar abundances of nuclei. However, there are a number of elements that can only be produced via processes involving proton rich nuclei. The rapid proton capture o ... More
Presented by Andrew M. ROGERS on 11 Sep 2009 at 09:40
Session: gamma-process I
The neutron capture cross sections of proton-rich nuclei are important for the nucleosynthesis of the heavy elements in the p process. Aspects of (n,gamma) reactions in the p process refer to the competition with (gamma,n) reactions, which affects the photodisintegration flux towards lighter nuclei, and to the formation of the final p-process abundances during the freeze-out phase. However, the kn ... More
Presented by Justyna MARGANIEC on 10 Sep 2009 at 14:50
Session: The nu~p process
Recent hydrodynamic simulations of core-collapse supernovae with accurate neutrino transport suggest that the bulk of the neutrino-heated ejecta is proton rich, in which the production of some interesting proton-rich nuclei is expected. However, there are a number of beta-waiting points that prevent the production of heavy proton-rich nuclei beyond iron in explosive events such as core-colla ... More
Presented by Shinya WANAJO on 11 Sep 2009 at 11:45
Session: rp-process
Presented by Anuj PARIKH on 11 Sep 2009 at 09:00
We have performed p-process simulations with an updated version of the Basel reaction library [1,2] including all (n,gamma) cross sections from the Karlsruhe Astrophysical Database in Stars project (v0.2) [3]. The simulations were carried out with a parametrized supernova type II shock front model (‘gamma -process’) of a 25 solar mass star and compared to recently published results of Rapp et ... More
Presented by Iris DILLMANN on 11 Sep 2009 at 12:15