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 plane PROBABILITY DISTRIBUTION

124 Sn + 64 Ni (35AMeV) b- impact parameter.  plane PROBABILITY DISTRIBUTION. Transversal velocity (v x ) reduction with increasing b. 124. 64. Sn +. Ni 35 MeV/nucl. 1.5. AH/AL= 4.6-10. E. =2700-3100. 2F. exp. 1.4. theo. Filtered. 1.3. <V_R>. 1.2. 1.1.

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 plane PROBABILITY DISTRIBUTION

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  1. 124Sn + 64Ni (35AMeV) b- impact parameter planePROBABILITY DISTRIBUTION Transversal velocity (vx) reduction with increasing b

  2. 124 64 Sn + Ni 35 MeV/nucl. 1.5 AH/AL= 4.6-10 E =2700-3100 2F exp 1.4 theo Filtered 1.3 <V_R> 1.2 1.1 1.0 -180 -150 -120 -90 -60 -30 0 30 60 90 120 150 180 F plane Preliminary Th. (No Filter included)

  3. E.Piasecki et al. IWM(2001) November 28, Catania(I) (preliminary)

  4. 124Sn+64Ni 35AMeV asystiff r DEPENDENCE OF IMF ISOSPIN COMPOSITION: EOS INFLUENCE asysoft 124Sn 64Ni

  5. ISOSCALINGand SYMMETRY ENERGY Isoscaling result: lnR21=Ct+N+Z  Interpretation: ; Consequences: 1.) for 2.) for 3.) always Yes, if Derivation of ? measured From Mirror Isobar Yield Ratios! Observations: - too large N/Z for both n-rich and n-poor systems - too small value for Problems: Evaporation corrections, Equilibrium scenario Heavier IMF’s – liquid phase ?

  6. NECK ISOSCALING Z=1 Z=2 Z=6 Z=7 Z=3 Z=5 Z=4 lnR21 Z=9 Z=8 N  = 0.95 asystiff asysoft  = 0.69 at 35 MeV/n (b=6,7,8fm)

  7. NECK ISOSCALING N=4 N=7 N=8 N=6 N=5 ln R21 N=2 N=3 Z asystiff  = -1.07 at 35 MeV/n (b=6,7,8fm) asysoft  = -0.68 “GRAND CANONICAL” NECK?

  8. Dynamical Isoscaling primary 50 AMeV (central coll.) Z=1 Z=7 final not very sensitive to Esym ? 124Sn Carbon isotopes (primary) M.J. van Goethem, G. Verde,M. Colonna MSU data (2001-02) Asy-stiff nucl-ex/0210004 Asy-soft A

  9. ISOSPIN IN REACTIONS: EOS – SENSITIVE OBSERVABLES • Competition of dissipative reaction mechanisms • N/Z of fast particle emission • (n,p) correlation functions • Isospin fractionation (isoscaling) * • Fragment multiplicities * • Isospin content of neck fragments * • Fast fission multiplicities • Isospin diffusion (charge equilibration) • n – p collective flows light isobar flows * • -/+yields * • Deconfinement precursors • n-radii, n-star cooling, hybrid stars * Asy-stiff indications but low asymmetries so far

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