NUCLEAR MANY-BODY THEORY AT FINITE TEMPERATURE APPLIED TO A PROTONEUTRON STAR

We describe the structure of the Sommerfeld approximation to the Walecka model. The approximation is also applied to an extended version of the Boguta and Bodmer model which takes hyperon and lepton degrees of freedom into account, including trapped neutrinos. We apply the results to the protoneutron star problem.

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A NUCLEAR MANY-BODY THEORY AT FINITE TEMPERATURE APPLIED TO A PROTONEUTRON STAR

International Journal of Modern Physics E ◽

10.1142/s0218301302000727 ◽

2002 ◽

Vol 11 (02) ◽

pp. 83-104 ◽

Cited By ~ 16

Author(s):

GUILHERME F. MARRANGHELLO ◽

CESAR A. Z. VASCONCELLOS ◽

MANFRED DILLIG ◽

J. A. DE FREITAS PACHECO

Keyword(s):

Phase Transition ◽

Nuclear Matter ◽

Finite Temperature ◽

Degrees Of Freedom ◽

Many Body ◽

Many Body Theory ◽

The Masses ◽

Protoneutron Stars ◽

Protoneutron Star

Thermodynamical properties of nuclear matter are studied in the framework of an effective many-body field theory at finite temperature, considering the Sommerfeld approximation. We perform the calculations by using the nonlinear Boguta and Bodmer model, extended by the inclusion of the fundamental baryon octet and leptonic degrees of freedom. Trapped neutrinos are also included in order to describe protoneutron star properties through the integration of the Tolman–Oppenheimer–Volkoff equations, from which we obtain, beyond the standard relations for the masses and radii of protoneutron stars as functions of the central density, new results of these quantities as functions of temperature. Our predictions include: the determination of an absolute value for the limiting mass of protoneutron stars; new structural aspects on the nuclear matter phase transition via the behavior of the specific heat and, through the inclusion of quark degrees of freedom, the properties of a hadron-quark phase transition and hybrid protoneutron stars

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From deuterons to neutron stars: variations in nuclear many-body theory

Reviews of Modern Physics ◽

10.1103/revmodphys.65.231 ◽

1993 ◽

Vol 65 (1) ◽

pp. 231-242 ◽

Cited By ~ 33

Author(s):

R. B. Wiringa

Keyword(s):

Neutron Stars ◽

Many Body ◽

Many Body Theory ◽

Body Theory ◽

Nuclear Many Body Theory

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Towards a unified description of the electroweak nuclear response

International Journal of Modern Physics E ◽

10.1142/s0218301315300064 ◽

2015 ◽

Vol 24 (06) ◽

pp. 1530006 ◽

Cited By ~ 6

Author(s):

Omar Benhar ◽

Alessandro Lovato

Keyword(s):

Cross Sections ◽

Compact Stars ◽

Kinematical Region ◽

Many Body ◽

Unified Framework ◽

Many Body Theory ◽

Atomic Nuclei ◽

Set Up ◽

Body Theory ◽

Nuclear Many Body Theory

We briefly review the growing efforts to set up a unified framework for the description of neutrino interactions with atomic nuclei and nuclear matter, applicable in the broad kinematical region corresponding to neutrino energies ranging between few MeV and few GeV. The emerging picture suggests that the formalism of nuclear many-body theory (NMBT) can be exploited to obtain the neutrino-nucleus cross-sections needed for both the interpretation of oscillation signals and simulations of neutrino transport in compact stars.

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55 YEARS OF THE SHELL MODEL: A CHALLENGE TO NUCLEAR MANY-BODY THEORY

International Journal of Modern Physics E ◽

10.1142/s0218301305003570 ◽

2005 ◽

Vol 14 (06) ◽

pp. 821-844 ◽

Cited By ~ 7

Author(s):

IGAL TALMI

Keyword(s):

Shell Model ◽

Wave Functions ◽

Many Body ◽

Apparent Absence ◽

Model Calculations ◽

Many Body Theory ◽

Body Theory ◽

Nuclear Many Body Theory ◽

Closed Shells ◽

Good Agreement

Shell model calculations of nuclear energies and wave functions of nucleons outside closed shells interacting by effective two-body forces yield good agreement with much experimental data. Many attempts have been made to calculate nuclear energies ab initio, by starting from some form of an interaction between free nucleons. Recent results of such calculations claim to obtain reasonable agreement with measured energies. These results, however, are obtained for wave functions which are very complicated. It is difficult to see how such wave functions are consistent with independent nucleon motion, the very essence of the shell model. In some of those calculations, 3-body interactions play a very important role. This is puzzling since nuclear energies are accurately obtained in shell model calculations by using only effective two-body interactions. In this paper, some examples of simple shell model calculations are reviewed. They exhibit good agreement with experiment and the apparent absence of the need for effective 3-body interactions.

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