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THE ASSOCIATED  PRODUCTION AND THE NUCLEAR INTERACTION OF  HYPERONS

J.Dąbrow s ki & J.Rożynek A.Sołtan Institute fot Nuclear Problems Kazimierz 2006. THE ASSOCIATED  PRODUCTION AND THE NUCLEAR INTERACTION OF  HYPERONS. Sources of information on V N : Associated production of Σ Strangeness exchange reactions  atoms

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THE ASSOCIATED  PRODUCTION AND THE NUCLEAR INTERACTION OF  HYPERONS

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  1. J.Dąbrowski & J.Rożynek A.Sołtan Institute fot Nuclear Problems Kazimierz 2006 THE ASSOCIATED  PRODUCTION AND THE NUCLEAR INTERACTION OF  HYPERONS Sources of information on VN : Associated production of Σ Strangeness exchange reactions  atoms N scattering

  2. Associated production PK+ P,  K,  P p- θ

  3. VP0 = 46 MeVVPls= 15 MeVR = 3.8 fm adjusted to proton separation energy and to the energies of the p1/2, p3/2, and s1/2 tates determined in (p,2p) and (e,e’) reactioms W0  P<kPOPN> W0  2.5 MeV

  4. Kaon spectrum from (-,K=) on 28Si at K=6o at p=1.2 GeV/c. Data from P.K.Saha, et al., Phys.Rev.C 70, 044612(2004). A V 0 = -20 MeV BV 0 = 20 MeV C V 0 = 40 MeV D V 0= 90 MeV E V 0= 100 MeV [ MeV ]

  5. Strangeness exchange reaction P+ P, K ,  PK p- θ

  6. VΣ(r)=VΣ0 θ(R-r) VΣ0=20 MeV VΣ0=10 MeV VΣ0= - 10/20 MeV Π+ spectrum in the (K-,π+) Brookhaven experiments. R. Sawafta, Nucl. Phys. A585, 103c (1995); S.Bart et al., Phys.Rev.Lrtt. 83, 5238 (1999). JD and J.Rozynek, Acta Phys. Pol. 29B, 2147 (1998).

  7. Σ ATOMSCoulomb Coulomb + strong Γ Γ ε Γ

  8.  ATOMS  Σ Atoms JD, J.Rozynek, G.S.Agnostatos, Eur.Phys.Journ.A 14, 125 (2002). {-(h2/2)-VC(r)+V(r)+iW(r)}= (E-iΓ/2) LDA V((r))+iW ((r))  –<kN> {-(h2/2) -VC(r) }0 = E00 energy shift  = Eo - E width 

  9. The Nijmegen N Interaction VN VN(models D, F, SC, NSC ) LOB Yamamoto et al. Progr.Theor.Phys. Suppl. 117, 241 (1994) VN() (effective interaction) JD Phys.ReV.C 60, 025205 (1992) V()

  10. V0for Nijmegen models D,F,SC,NSC JD Nucl.Phys. A691,58c (2001).

  11. Summary • Our simple analysis of the associated production data suggests that the  s.p. potential U inside the nuclear core is stronglyrepulsive ( ~ 100 MeV).* • On the other hand a similar analysis of the strangeness exchange data and our analysis of the  atomic data suggests that at nuclear matter densities appearing inside nuclei. U is lessrepulsive ( ~ 20 MeV). • Astrophysical consequences: • stiffer EOS  greater masses of neutron stars

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