Göttingen 1997 – wissenschaftliches Programm
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HK: Hadronen und Kerne
HK 16: Nukleare Astrophysik I
HK 16.7: Vortrag
Montag, 24. März 1997, 18:45–19:00, HS H
Implications of the new ETFSI-Q mass formula on r-process abundances ∗ — •B. Pfeiffer1, K.-L. Kratz1, F.-K. Thielemann2, and J. Dobaczewski3 — 1Institut für Kernchemie, Universität Mainz, Germany — 2Institut für Theoretische Physik, Universität Basel, Switzerland — 3Institute of Theoretical Physics, Warsaw University, Poland
The implications of the new ETFSI-Q mass formula [1] with Bogolyubov-enhanced shell-quenching [2] on reproducing the solar-system r-process abundances (Nr,⊙) are studied within the waiting-point approximation. Compared to the results obtained with earlier macroscopic-microscopic masses as ETFSI-1 and FRDM [3], a considerable improvement of the global Nr,⊙ fit is obtained. With this new approach, predictions are made for the r-abundances of the heaviest isotopes beyond the A≃195 peak (i.e. 203Tl to 209Bi) and of the long-lived r-process cosmochronometers 232Th, 235,238U and 244Pu, which are for the first time based on internally consistent nuclear-physics input data.
[1] J. M. Pearson et al., Phys. Lett. B, in press
[2] J. Dobaczewski et al., Phys. Scr. T56, 15 (1995)
[3] K.-L. Kratz et al., Astrophys. J. 403, 216 (1993) ∗ work supported by the GSI Hochschulprogramm and the BMBF (06MZ465)