Nuclear matter
Nuclear physics |
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Nuclear matter is an idealized system of interacting nucleons (
Infinite volume implies no surface effects and translational invariance (only differences in position matter, not absolute positions).A common idealization is symmetric nuclear matter, which consists of equal numbers of protons and neutrons, with no electrons.
When nuclear matter is compressed to sufficiently high density, it is expected, on the basis of the
Some authors use "nuclear matter" in a broader sense, and refer to the model described above as "infinite nuclear matter",[1] and consider it as a "toy model", a testing ground for analytical techniques.[8] However, the composition of a neutron star, which requires more than neutrons and protons, is not necessarily locally charge neutral, and does not exhibit translation invariance, often is differently referred to, for example, as neutron star matter or stellar matter and is considered distinct from nuclear matter.[9][10] In a neutron star, pressure rises from zero (at the surface) to an unknown large value in the center.
Methods capable of treating finite regions have been applied to stars and to atomic nuclei.[11][12] One such model for finite nuclei is the liquid drop model, which includes surface effects and Coulomb interactions.
See also
- QCD vacuum
- Quark–gluon plasma
- Degenerate matter
- Neutron-degenerate matter
- Strange matter
- Nuclear structure
- Neutronium
- Nuclear physics
- Nuclear spectroscopy
References
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Dominique Durand; Eric Suraud; Bernard Tamain (2001). Nuclear dynamics in the nucleonic regime. ISBN 0-7503-0537-1.
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Richard D. Mattuck (1992). A Guide to Feynman Diagrams in the Many-body Problem (Reprint of 1974 McGraw-Hill second ed.). ISBN 0-486-67047-3.
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ISBN 981-238-898-2.
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Helmut Hofmann (2008). The Physics of Warm Nuclei: With Analogies to Mesoscopic Systems. ISBN 978-0-19-850401-6.
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Stefan B Rüster (2007). "Phase diagram of neutral quark matter at moderate densities". In Armen Sedrakian; John Walter Clark; Mark Gower Alford (eds.). Pairing in fermionic systems. World Scientific. ISBN 978-981-256-907-3.
- ISBN 978-0-387-33543-8.
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Herbert Müther (1999). "Dirac-Brueckner approach for finite nuclei". In Marcello Baldo (ed.). Nuclear methods and the nuclear equation of state. World Scientific. p. 170. ISBN 981-02-2165-7.
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Francesca Gulminelli (2007). "Nuclear matter versus stellar matter". In A. A. Raduta; V. Baran; A. C. Gheorghe; et al. (eds.). Collective Motion and Phase Transitions in Nuclear Systems. World Scientific. ISBN 978-981-270-083-4.
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Norman K. Glendenning (2000). Compact stars (2 ed.). Springer. p. 242. ISBN 0-387-98977-3.
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F. Hofmann; C. M. Keil; H. Lenske (2001). "Density dependent hadron field theory for asymmetric nuclear matter and exotic nuclei". Phys. Rev. C. 64 (3): 034314. S2CID 17453709.
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A. Rabhi; C. Providencia; J. Da Providencia (2008). "Stellar matter with a strong magnetic field within density-dependent relativistic models". J Phys G. 35 (12): 125201. S2CID 119098245.