Inhomogeneous nuclear matter in compact stars Kenichiro Nakazato - - PowerPoint PPT Presentation
Inhomogeneous nuclear matter in compact stars Kenichiro Nakazato Kyushu University International Symposium on Neutron Star Matter (NSMAT2016), November 23, 2016 Compact stars Supernova core core collapse supernova Proto-neutron
International Symposium on Neutron Star Matter (NSMAT2016), November 23, 2016
0.1n0 0.01n0
density
~ 3×1014 g/cm3 uniform matter clusters of nucleons （nuclei）
neutron proton
matter
density ↗ “Nuclei” “Hole nuclei”
Figure by K. Oyamatsu （1993）
meat ball spaghetti lasagna macaroni Swiss cheese
uniform matter
double gyroid single gyroid
u
c.f., Nakazato et al., PRL 103 (2009) 132501. Nakazato et al., PRC 83 (2011) 065811.
Yp = 0.3
Schuetrumpf et al., PRC 91 (2015) 025801
binding energy （MeV）
single gyroid
Supernova
high density inner low density
uniform inhomogeneous
T B Yp
NS EOS
Yp B
inhomogeneous @T = 0 0.5 B（g/cm3） 1014 106 0.01 100 T （MeV）
proton fraction Yp
Fischer+ (2011)
PNS cooling
– Lattimer & Swesty (1991) – Shen et al. (1998)
Togashi et al., submitted inhomogeneous
based on realistic nuclear force.
– Togashi & Takano (2013)
inhomogeneous phase with Thomas-Fermi approach.
– Oyamatsu (1993) Yp = 0.5 Yp = 0.01
– seen in symmetry energy Esym and gradient L.
Variational Shen EOS
E / N [MeV]
nB [fm-3]
Yp = 0.5 Yp = 0
– because of smaller symmetry gradient L.
New EOS Shen EOS PNS profile of 7s after the bounce, model from Nakazato et al. (2013) inner region