TY - GEN
T1 - Equation of State for Hadron-Quark Mixed Phase and Stellar Collapse
AU - Nakazato, Ken'Ichiro
AU - Sumiyoshi, Kohsuke
AU - Yamada, Shoichi
N1 - Funding Information:
We are grateful to Hideyuki Umeda for providing a progenitor model. We would like to thank Akira Ohnishi and Chikako Ishizuka for fruitful discussions. Numerical computations were performed on the supercomputers in NAOJ, JAERI, YITP and KEK. This work was partially supported by JSPS Research Fellowship, Grants-in-Aid for the Scientific Research from the Ministry of Education, Science and Culture of Japan and the 21st-century COE Program at Waseda University.
Publisher Copyright:
© 2008 American Institute of Physics.
PY - 2008
Y1 - 2008
N2 - We construct an equation of state (EOS) including the hadron-quark phase transition by the Gibbs conditions for finite temperature. We adopt the equation of state based on the relativistic mean field theory for the hadronic phase taking into account pions and the MIT bag model of the deconfined 3-flavor strange quark matter for the quark phase. The gravitational collapse of a massive star is computed using our equation of state and we find that the interval time from the bounce to the black hole formation, namely the duration time of the neutrino emission, becomes shorter for the model with pions and quarks. This fact implies that we may be able to probe observationally the EOS of hot dense matter in future.
AB - We construct an equation of state (EOS) including the hadron-quark phase transition by the Gibbs conditions for finite temperature. We adopt the equation of state based on the relativistic mean field theory for the hadronic phase taking into account pions and the MIT bag model of the deconfined 3-flavor strange quark matter for the quark phase. The gravitational collapse of a massive star is computed using our equation of state and we find that the interval time from the bounce to the black hole formation, namely the duration time of the neutrino emission, becomes shorter for the model with pions and quarks. This fact implies that we may be able to probe observationally the EOS of hot dense matter in future.
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U2 - 10.1063/1.2943586
DO - 10.1063/1.2943586
M3 - Conference contribution
AN - SCOPUS:85036502525
T3 - AIP Conference Proceedings
SP - 282
EP - 287
BT - Origin of Matter and Evolution of Galaxies - 10th International Symposium on Origin of Matter and Evolution of Galaxies
A2 - Kajino, Toshitaka
A2 - Suda, Takuma
A2 - Nozawa, Takaya
A2 - Ohnishi, Akira
A2 - Fujimoto, Masayuki Y.
A2 - Kubono, Shigeru
A2 - Kato, Kiyoshi
PB - American Institute of Physics Inc.
T2 - 10th International Symposium on Origin of Matter and Evolution of Galaxies: From the Dawn of Universe to the Formation of Solar System, OMEG 2007
Y2 - 4 December 2007 through 7 December 2007
ER -