Cold pasta phase in the extended Thomas–Fermi approximation

2015 ◽  
Vol 24 (10) ◽  
pp. 1550078 ◽  
Author(s):  
S. S. Avancini ◽  
B. P. Bertolino
Keyword(s):  
Neutron Stars ◽  
Transition Density ◽  
Zero Temperature ◽  
Thomas Fermi ◽  
Walecka Model

In this paper, we aim to obtain more accurate values for the transition density to the homogenous phase in the nuclear pasta that occurs in the inner crust of neutron stars. To that end, we use the nonlinear Walecka model at zero temperature and an approach based on the extended Thomas–Fermi (ETF) approximation.

TOWARDS A RELATIVISTIC THOMAS-FERMI THEORY OF WHITE DWARFS AND NEUTRON STARS

2011 ◽  
Vol 20 (supp01) ◽  
pp. 141-148
Author(s):  
JORGE A. RUEDA ◽  
REMO RUFFINI
Keyword(s):  
Neutron Stars ◽  
White Dwarfs ◽  
Recent Progress ◽  
Fermi Theory ◽  
Thomas Fermi ◽  
General Relativistic

We summarize recent progress in the formulation of a theory for white dwarfs and neutron stars based on the general relativistic Thomas-Fermi equations of equilibrium.

scholarly journals Thomas‐Fermi Calculations of Atoms and Matter in Magnetic Neutron Stars. II. Finite Temperature Effects

1998 ◽  
Vol 502 (2) ◽  
pp. 847-857 ◽  
Author(s):  
A. Thorolfsson ◽  
O. E. Rognvaldsson ◽  
J. Yngvason ◽  
E. H. Gudmundsson
Keyword(s):  
Neutron Stars ◽  
Finite Temperature ◽  
Temperature Effects ◽  
Thomas Fermi

scholarly journals Constraints on the inner edge of neutron star crusts from relativistic nuclear energy density functionals

2019 ◽  
Vol 18 ◽  
pp. 107
Author(s):  
Ch. C. Moustakidis ◽  
T. Niksic ◽  
G. A. Lalazissis ◽  
D. Vretenar ◽  
P. Ring
Keyword(s):  
Neutron Star ◽  
Energy Density ◽  
Neutron Stars ◽  
Nuclear Energy ◽  
Liquid Core ◽  
Transition Density ◽  
Binding Energies ◽  
Density Functionals ◽  
The Core ◽  
Finite Nuclei

The transition density nt and pressure Pt at the inner edge between the liquid core and the solid crust of a neutron star are analyzed using the thermodynami- cal method and the framework of relativistic nuclear energy density functionals. Starting from a functional that has been carefully adjusted to experimental binding energies of finite nuclei, and varying the density dependence of the cor- responding symmetry energy within the limits determined by isovector prop- erties of finite nuclei, we estimate the constraints on the core-crust transition density and pressure of neutron stars: 0.086 fm−3 ≤ nt < 0.090 fm−3 and 0.3 MeV fm−3 < Pt ≤ 0.76 MeV fm−3 [1].

scholarly journals Relativistic Neutron Stars: Rheological Type Extensions of the Equations of State

Symmetry ◽  
2019 ◽  
Vol 11 (2) ◽  
pp. 189
Author(s):  
Alexander Balakin ◽  
Alexei Ilin ◽  
Anna Kotanjyan ◽  
Levon Grigoryan
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Equations Of State ◽  
Pressure Profile ◽  
Spherically Symmetric ◽  
Zero Temperature ◽  
New Approach ◽  
Modified Equations

Based on the Rheological Paradigm, we extend the equations of state for relativistic spherically symmetric static neutron stars, taking into consideration the derivative of the matter pressure along the so-called director four-vector. The modified equations of state are applied to the model of a zero-temperature neutron condensate. This model includes one new parameter with the dimensionality of length, which describes the rheological type screening inside the neutron star. As an illustration of the new approach, we consider the rheological type generalization of the non-relativistic Lane–Emden theory and find numerically the profiles of the pressure for a number of values of the new guiding parameter. We have found that the rheological type self-interaction makes the neutron star more compact, since the radius of the star, related to the first null of the pressure profile, decreases when the modulus of the rheological type guiding parameter grows.

Proto-neutron stars in the Thomas-Fermi theory

2019 ◽  
Vol 986 ◽  
pp. 133-149 ◽  
Author(s):  
M. Ghazanfari Mojarrad ◽  
N.S. Razavi
Keyword(s):  
Neutron Stars ◽  
Fermi Theory ◽  
Thomas Fermi

ON THE EINSTEIN–MAXWELL–THOMAS–FERMI EQUATIONS OF EQUILIBRIUM FOR WHITE DWARFS AND NEUTRON STARS

2013 ◽  
Vol 22 (11) ◽  
pp. 1360007 ◽  
Author(s):  
JORGE A. RUEDA ◽  
REMO RUFFINI
Keyword(s):  
Neutron Stars ◽  
Maxwell Equations ◽  
White Dwarfs ◽  
Recent Progress ◽  
Thomas Fermi ◽  
General Relativistic

We summarize recent progress in the formulation of a theory for white dwarfs and neutron stars taking into account the strong, weak, electromagnetic and gravitational interactions based on the general relativistic Thomas–Fermi equations of equilibrium and the Einstein–Maxwell equations.

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