Relativistic EOS table including hyperons and pions
Tables of Hyperonic Matter Equation of State for Core-Collapse Supernovae
*** INTRODUCTION ***
As you know, baryons having strangness (heyrons) exist
in dense matter like high density supernova explosion environment,
neutrons stars, or early stage of blackhole. Today, we can
obtain the basic information on hyperon-nucleon (YN) interaction
at around normal nuclear density through pion induced heavy ion
collision at KEK etc. Then we know Lambda-N, Xi-N interaction at the
normal density from such a recent progress in strengeness nuclear
physcs. However, unfortunately, Sigma-N interaction has a large
ambiguity even at present. This difference of Sigma-N interaction
results in different components of dense matter and the stiffness of
EOS. Therefore, we provide various EOS tables within this Sigma-N
ambiguity as follows in this site. We wish this EOS tables
will be helpful to your study.
*** RELATIVISITC EOS TABLE ***
We adopt these YN interaction:
Lamda-N = -30MeV, Xi-N = -15MeV, Siga-N=(-30 to +90)MeV.
The most recomended Sigma-N interaction is +30 MeV
at normal density.
These EOS tables contain the same information as Shen EOS table, physical quantities such as
pressure, energy, or somethig like that, follow the Shen EOS notation
and units. Therefore if you have already used Shen EOS table,
you can apply these EOS tables to your calculations.
The following compressed directories are made of two files
--- "####.tbl" and "####.urt".
"####.tbl" means EOS table in Shen EOS table style,
while you can see particle ratios at each (Ye, rhoB, T) in "####.urt".
Here, the (Ye, rhoB, T) conditions are decided by Shen EOS tables.
The former four files consist of only nucleons and hyperons,
thermal pion contributions are added to the latter four files.
*** README ***
You can see the detail of our EOS in Jornal of Physics G:
Nucl.Part.Phys.35085201(19pp),2008
nucl-th/0802.2318v3
Simulation of black-hole formation with this EOS was performed by Sumiyoshi et al.
(NICX proceedings and ApJL 690 L43-L46, 2009)
nucl-th/0811.4237
If you have any questions and comments, please give Email to
Chikako Ishizuka
or
Akira Ohnishi
(gmail).