D
2007
Nuclear Matter Equations of State and the Neutron Stars
BĚTÁK, Emil, Zdeněk STUCHLÍK and Martin URBANEC
Basic information
Original name
Nuclear Matter Equations of State and the Neutron Stars
Edition
Melville, New York, Frontiers in Nuclear Structure, Astrophysics, and Reactions Finustar 2, p. 313-317, 4 pp. 2007
Other information
Type of outcome
Stať ve sborníku
Field of Study
10308 Astronomy
Confidentiality degree
není předmětem státního či obchodního tajemství
Organization unit
Faculty of Philosophy and Science in Opava
Keywords in English
Asymmetric nuclear matter, Neutron stars, Quantum hydrodynamics, Relativistic Brueckner-Hartree-Fock, Equations of state
Tags
International impact
Links
LC06014, research and development project. MSM4781305903, plan (intention).
V originále
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.
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