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Milan MATOŠ

Milan MATOŠ. TOF Mass Measurements at the Extremes: An input for astrophysical calculations. Principle of TOF Mass Measurements. B r. usually B r acceptance ± several percent. solutions. B r measurement. isochronicity. t constant for fixed m/q even if v 1 < v 2.

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Milan MATOŠ

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  1. Milan MATOŠ TOF Mass Measurements at the Extremes: An input for astrophysical calculations

  2. Principle of TOF Mass Measurements Br usually Br acceptance ± several percent solutions Br measurement isochronicity t constant for fixed m/q even if v1 < v2 dispersive mode

  3. Isochronous Mass Measurement in the Storage Ring at GSI 10m

  4. Time-of-Flight Measurement with the Storage Ring in the Isochronous Mode

  5. Measured Masses of Uranium Fission Fragments

  6. TOF-B Mass Measurement at THE NSCL r

  7. known mass Results very well known mass s<30keV

  8. known mass Results very well known mass s<30keV ISOLTRAP N>1000 LEBIT

  9. Preliminary Fit fit of the reference masses m/q = function(TOF, Z) VERY PRELIMINARY Comparison with Mass Models AME extrapolation VERY PRELIMINARY new measured mass value only statistical uncertainties!!! Ni isotopes

  10. Thanks Alfredo Estrade, Hendrik Schatz, Daniel Bazin, Alexandra Gade, Daniel Galaviz, Giuseppe Lorusso, Mauricio Portillo, Dan Shapira, Andreas Stolz, John Yurkon, Mark Wallace and many others NSCL, MSU & JINA & ORNL & LANL & Ohio Univ.

  11. preceding following Astrophysical Motivation • after enormous interest in explosive processes in stars • sites still not clear • last decade rise of the interest in processes: the explosions

  12. r-process conditions Only np-, a- process r-process Seed Nuclei in Neutrino-Driven Wind Model of Core-Collapsed Supernovae • high temperature ejecta • cooled by adiabatic expansion • driven by a neutrino wind n, p, a charge-particle freeze-out Calculations: K. Farouqi, F. Montes et al. FRDM mass model used need of nuclear physics data Area covered in this experiment seed/n too high

  13. electron Fermi energy Heating of the Accreting Neutron Star Crust(after rp-process) • after matter flow suppressed • ashes of rp-process sink deeper into the crust, • me rises with an increasing density • Haensel & Zdunik: on a single rp-process nuclide • two stages electron capture • n emission and absorption • pycnonuclear fusion r>1012g/cm2 calculated excitation energies • Schatz, Cumming: • superburst: 12C ignition at r ~109g/cm2 • not enough heat according to HZ model! • S. Gupta et al: on realistic rp-ashes mix • electron capture into excited states followed • by a radiative deexcitation – more heat! masses needed for reaction thresholds, separation energies and reaction rates FRDM (Möller et al., 1995) used S. Gupta et al. astro-ph/0609828

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