Nuclear Matter Equations of State and the Neutron Stars

@inproceedings{43062,
   author = {Běták, Emil and Stuchlík, Zdeněk and Urbanec, Martin},
   address = {Melville, New York},
   booktitle = {Frontiers in Nuclear Structure, Astrophysics, and Reactions Finustar 2},
   doi = {http://dx.doi.org/10.1063/1.2939317},
   keywords = {Asymmetric nuclear matter, Neutron stars, Quantum hydrodynamics, Relativistic Brueckner-Hartree-Fock, Equations of state},
   language = {eng},
   location = {Melville, New York},
   isbn = {978-0-7354-0532-5},
   pages = {313-317},
   title = {Nuclear Matter Equations of State and the Neutron Stars},
   year = {2007}
}

TY  - JOUR
ID  - 43062
AU  - Běták, Emil - Stuchlík, Zdeněk - Urbanec, Martin
PY  - 2007
TI  - Nuclear Matter Equations of State and the Neutron Stars
CY  - Melville, New York
SN  - 9780735405325
KW  - Asymmetric nuclear matter, Neutron stars, Quantum hydrodynamics, Relativistic Brueckner-Hartree-Fock, Equations of state
N2  - The equations of state (EoS) of relativistic asymmetric nuclear matter are obtainable from assumed form of the interaction Lagrangian. They are one of important inputs to describe the neutron stars. The structure of the neutron stars , i.e. the density of matter and the pressure as functions of radial distance starting from their values at the center of a star, is straightforwardly dependent on EoS. Similarly, a limitation on the total mass of the neutron star can be obtained therefrom. Thus, EoS and the underlying nucleon interactions can be tested also by the means of astronomical observations.
ER  - 

BĚTÁK, Emil, Zdeněk STUCHLÍK a Martin URBANEC. Nuclear Matter Equations of State and the Neutron Stars. In \textit{Frontiers in Nuclear Structure, Astrophysics, and Reactions Finustar 2}. Melville, New York, 2007, s.~313-317, 4 s. ISBN~978-0-7354-0532-5. Dostupné z: https://dx.doi.org/10.1063/1.2939317.