Tübingen 2003 – wissenschaftliches Programm
Bereiche | Tage | Auswahl | Suche | Downloads | Hilfe
HK: Physik der Hadronen und Kerne
HK 21: Kern- und Teilchen-Astrophysik II
HK 21.5: Vortrag
Dienstag, 18. März 2003, 16:45–17:00, F
Canonical r-process calculation: comparison of different mass models — •Uwe Heinzmann1, K-L. Kratz1, B. Pfeiffer1, K. Farouqi1, K. Vaughan2, A. Aprahamian2, and F-K. Thielemann3 — 1Inst. f. Kernchemie, Univ. Mainz — 2Dept. of Physics, Univ. of Notre Dame — 3Dept. f. Physik & Astronomie, Univ. Basel
In our r-process calculations we use different mass models, which are in general (macroscopic-) microscopic approaches. The development towards selfconsistent models is still in progress; hence we expect to obtain an increasingly realistic picture of the r-process. The mass formulae we use are the Finite Range Droplet Model (FRDM) [1], two versions based on the Extended Thomas-Fermi plus Strutinsky Integral approach (ETFSI-1, ETFSI-Q) [2], [3] and three models based on the HF and HFB methods (HFB/SkP, HFBCS-1, HFB-2) [4][5][6]. In our systematic parameter studies we mainly focus on the r-process behavior in the regions of the magic neutron shells ( N=50, 82, 126); i.e. the r-matter flow to build up the r-abundance peaks and the breakout from the magic-shell waiting-point nuclides. From these studies we deduce the astrophysical parameters (temperature, neutron density, process duration) required to reproduce the global solar-system r-abundance pattern.
[1] P. Möller et al. ADNDT 59 (1995) 185
[2] Y. Aboussir et al., ADNDT 61 (1995) 127
[3] J. M. Pearson et al., Phys. Lett. B 387 (1996) 455
[4] J. Dobaczewski et al., Phys. Scripta T 56 (1995) 15
[5] S. Goriely et al., ADNDT 77 (2001) 311
[6] M. Samyn et al., Nucl. Phys. A 700 (2001) 142