Equation of State of Dense Matter with Trapped Neutrinos

  • A chiral hadronic model is extended to investigate the influences of trapped neutrinos on the equation of state of dense matter and structure of protoneutron stars. Our results show that trapped neutrinos lead to the increase of proton fraction and make the equation of state of dense matter soft. Furthermore, maximum masses and radii of protoneutron stars decrease when neutrinos are trapped.
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ZHOU Ran and GUO Hua. Equation of State of Dense Matter with Trapped Neutrinos[J]. Chinese Physics C, 2004, 28(1): 26-29.
ZHOU Ran and GUO Hua. Equation of State of Dense Matter with Trapped Neutrinos[J]. Chinese Physics C, 2004, 28(1): 26-29. shu
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Received: 2003-04-14
Revised: 1900-01-01
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Equation of State of Dense Matter with Trapped Neutrinos

    Corresponding author: GUO Hua,
  • Department of Technical Physics,and MOE Laboratory of Heavy Ion Physics,Peking University,Beijing 100871,China2 Center of Theoretical Nuclear Physics,National Laboratory of Heavy Ion Accelerator,Lanzhou 730000,China

Abstract: A chiral hadronic model is extended to investigate the influences of trapped neutrinos on the equation of state of dense matter and structure of protoneutron stars. Our results show that trapped neutrinos lead to the increase of proton fraction and make the equation of state of dense matter soft. Furthermore, maximum masses and radii of protoneutron stars decrease when neutrinos are trapped.

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