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Astron. Astrophys. Suppl. Ser. 134, 39-52

Thermal history and structure of rotating protoneutron stars with relativistic equation of state

K. Sumiyoshi 1 - J.M$^{\underline{\mbox{a}}}$ Ibáñez 2 - J.V. Romero 3

Send offprint request: J.V. Romero

1 - The Institute of Physical and Chemical Research, (RIKEN), Wako, Saitama 351-01, Japan
2 - Departamento de Astronomía y Astrofísica, Universidad de Valencia, 46100 Burjassot, Spain
3 - Departamento de Matemática Aplicada, Universidad Politécnica de Valencia, 46071 Valencia, Spain

Received March 17; accepted July 7, 1998


We study the properties of general relativistic, slowly rotating, protoneutron stars. We explore the structure of rotating protoneutron stars with a wide range of the entropy per baryon, the lepton fraction and the baryonic mass in order to study the evolutionary history of protoneutron stars during the cooling epoch. We adopt the relativistic equation of state for dense matter derived within the relativistic mean field theory, which is based on the microscopic nuclear many-body framework, and checked by the experimental data of many nuclei. We provide broad information on the effect of rotation, temperature and lepton trapping of protoneutron stars with various baryonic masses. The evolutionary track of rotating protoneutron stars is examined and its implications are addressed.

Key words: dense matter -- stars: interiors -- stars: neutron -- stars: rotation

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