The structure of a proto-neutron star. Chung- Yeol Ryu Hanyang University, Korea. C.Y.Ryu , T.Maruyama,T.Kajino , M.K.Cheoun , PRC2011. C.Y.Ryu , T.Maruyama,T.Kajino , G.J.Mathews , M.K.Cheoun , PRC2012 . Outline 1. Introduction 2. Motivations 3. Models and conditions
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a proto-neutron star
Hanyang University, Korea
C.Y.Ryu, T.Maruyama,T.Kajino, M.K.Cheoun, PRC2011.
C.Y.Ryu, T.Maruyama,T.Kajino, G.J.Mathews, M.K.Cheoun, PRC2012.
3. Models and conditions
The depiction of a Shapiro Delay
The structure of supernovae
The production of proto-neutron star
Burrows&Lattimer APJ (1981), APJ(1987)
without convection with convection
S. Reddy et al. PRD(1998)
S. Reddy et al. PRD(1998) A. Burrows’ simulation
n + νe p + e- :
Thermodynamic potential Ω
- Minimum condition
Microscopic model: Hamiltonian or Lagangian
Grand partition function Z
at saturation density
Energy per nucleon in symmetric matter
Energy per nucleon in asymmetric matter
Nucleons (Dirac equation)
meson fields (Klein-Gordon equation)
Meson fields mean fields (notransition)
Isentropic process : S = 2 (S : entropy per a baryon)
where x is trapped ratio.
Static and spherical symmetric neutron star (Schwarzschild metric)
Static perfect fluid
Diag Tμν = (ε, p, p, p)
QHD & QMC models
-Eq. of motion
Cold NS(T=0) Proto-NS(S=2)
1. Proto-neutron star : After supernovae explosion, the initial state of NS is called PNS.
2. YL = 0.4 condition is not enough to explain trapped neutrino ratio.
3. So, we introduce that the trapped ratio may depend on the baryon densities.
- The results agree with simulation.
4. The moment of inertia : PNS CNS
- Pulsar rotation may depend on the mass.