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

1993 ◽  
Vol 65 (1) ◽  
pp. 231-242 ◽  
Author(s):  
R. B. Wiringa
Keyword(s):  
Neutron Stars ◽  
Many Body ◽  
Many Body Theory ◽  
Body Theory ◽  
Nuclear Many Body Theory

scholarly journals Towards a unified description of the electroweak nuclear response

2015 ◽  
Vol 24 (06) ◽  
pp. 1530006 ◽  
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.

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

2005 ◽  
Vol 14 (06) ◽  
pp. 821-844 ◽  
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.

A NUCLEAR MANY-BODY THEORY WITH TSALLIS STATISTICS

2003 ◽  
Author(s):  
A. MESQUITA ◽  
M. RAZEIRA ◽  
C.A.Z. VASCONCELLOS ◽  
H. T. COELHO ◽  
M. DILLIG ◽  
...  
Keyword(s):  
Many Body ◽  
Tsallis Statistics ◽  
Many Body Theory ◽  
Body Theory ◽  
Nuclear Many Body Theory

Unitary-model-operator approach to nuclear many-body theory

1994 ◽  
Vol 242 (1-3) ◽  
pp. 181-190 ◽  
Author(s):  
K. Suzuki ◽  
R. Okamoto ◽  
H. Kumagai
Keyword(s):  
Many Body ◽  
Model Operator ◽  
Operator Approach ◽  
Many Body Theory ◽  
Unitary Model ◽  
Body Theory ◽  
Nuclear Many Body Theory

scholarly journals Nuclear many-body theory for the study of QCD sum rules in matter

1995 ◽  
Vol 51 (6) ◽  
pp. 3372-3387 ◽  
Author(s):  
L. S. Celenza ◽  
C. M. Shakin ◽  
Wei-Dong Sun ◽  
J. Szweda
Keyword(s):  
Sum Rules ◽  
Many Body ◽  
Qcd Sum Rules ◽  
Many Body Theory ◽  
Body Theory ◽  
Nuclear Many Body Theory

A FAIR CHANCE FOR SUPERNOVAE

2007 ◽  
Vol 16 (04) ◽  
pp. 1107-1120
Author(s):  
KARLHEINZ LANGANGKE ◽  
G. MARTÍNEZ-PINEDO
Keyword(s):  
Nuclear Physics ◽  
Type Ii ◽  
Many Body ◽  
Many Body Theory ◽  
Interaction Processes ◽  
Finite Nuclei ◽  
Body Theory ◽  
Nuclear Many Body Theory ◽  
Fair Chance ◽  
Collapse Phase

Nuclear physics plays an essential role in the dynamics of a type II supernova (a collapsing star). Recent advances in nuclear many-body theory allow now to calculate the stellar weak-interaction processes involving nuclei. The most important process is the electron capture on finite nuclei with mass numbers A > 55. This process is the source of neutrinos during the collapse phase. Neutrino-nucleus reactions play an interesting role during the collapse and the supernova nucleosynthesis.

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