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Nuclear Theory·nucl-th

Wednesday·December 24, 2014

6 papers—2 primary·4 cross-listed

All6Primary2Cross-lists4
  1. 01

    [Submitted on 23 Dec 2014]

    Refractive effects and Airy structure in inelastic O+C rainbow scattering

    S. Ohkubo · Y. Hirabayashi · A. A. Ogloblin · Yu. A. Gloukhov · A. S. Dem'yanova · W. H. Trzaska

    Inelastic O +C rainbow scattering to the (4.44 MeV) state of C was measured at the incident energies, = 170, 181, 200, 260 and 281 MeV. A systematic analysis of the experimental angular distributions was performed using the coupled channels method with an extended double folding potential derived from realistic wave functions for C and O calculated with a microscopic cluster model and a finite-range density-dependent nucleon-nucleon force.The coupled channels analysis of the measured inelastic scattering data shows consistently some Airy-like structure in the inelastic scattering cross sections for the first state of C, which is somewhat obscured and still not clearly visible in the measured data. The Airy minimum was identified from the analysis and the systematic energy evolution of the Airy structure was studied. The Airy minimum in inelastic scattering is found to be shifted backward compared with that in elastic scattering.

    Comments:
    7 pages, 5 figures
    Subjects:
    Nuclear Theory (nucl-th)
    arXiv:
    1412.7239 [pdf]
    PRC(2014)·15 citations
  2. 02

    [Submitted on 23 Dec 2014]

    Anisotropic pressure and hyperons in neutron stars

    A. Sulaksono🇮🇩

    We study the effects of anisotropic pressure on properties of the neutron stars with hyperons inside its core within the framework of extended relativistic mean field. It is found that the main effects of anisotropic pressure on neutron star matter is to increase the stiffness of the equation of state, which compensates for the softening of the EOS due to the hyperons. The maximum mass and redshift predictions of anisotropic neutron star with hyperonic core are quite compatible with the result of recent observational constraints if we use the parameter of anisotropic pressure model [1] and [2]. The radius of the corresponding neutron star at =1.4 is more than 13 km, while the effect of anisotropic pressure on the minimum mass of neutron star is insignificant. Furthermore, due to the anisotropic pressure in the neutron star, the maximum mass limit of higher than 2.1 cannot rule out the presence of hyperons in the neutron star core.

    Comments:
    Int. J. Mod. Phys. E (accepted)
    Subjects:
    Nuclear Theory (nucl-th)
    arXiv:
    1412.7247 [pdf]
    IJMPE(2015)·35 citations

Affiliations

first authorsco-authorsvia INSPIRE