Rapidly Rotating Neutron Star Models: Erratum

1990 ◽  
Vol 351 ◽  
pp. 705 ◽  
Author(s):  
John L. Friedman ◽  
James R. Ipser ◽  
Leonard Parker
Keyword(s):  
Neutron Star ◽  
Star Models

scholarly journals Neutrinos in Proto-neutron Star Models

2013 ◽  
Vol 44 (11) ◽  
pp. 2389
Author(s):  
M. Pieńkos
Keyword(s):  
Neutron Star ◽  
Star Models ◽  
Proto Neutron Star

scholarly journals Dynamical Stability of Neutron Stars

1971 ◽  
Vol 46 ◽  
pp. 341-345
Author(s):  
G. Chanmugam ◽  
M. Gabriel
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Neutron Stars ◽  
Dynamical Stability ◽  
Star Models

The Nemeth-Sprung equation of state is modified and used to obtain neutron star models. Contrary to the results of some authors it is found that neutron stars with central densities ≲ 1014 g cm-3 are dynamically stable. It is suggested that some pulsars may belong to this category of stars.

Relativistic fluid spheres applicable to neutron star models

1978 ◽  
Vol 224 ◽  
pp. 993 ◽  
Author(s):  
P. G. Whitman ◽  
R. W. Redding
Keyword(s):  
Neutron Star ◽  
Star Models ◽  
Relativistic Fluid ◽  
Fluid Spheres

scholarly journals Einstein Observatory Limits on Neutron Star Surface Temperatures

1987 ◽  
Vol 125 ◽  
pp. 457-457
Author(s):  
F.R. Harnden
Keyword(s):  
Star Formation ◽  
Neutron Star ◽  
Neutron Stars ◽  
Supernova Remnants ◽  
Theoretical Models ◽  
X Ray ◽  
Star Models ◽  
Formation And Evolution ◽  
Star Surface ◽  
Einstein Observatory

For years the theoretical models of neutron star formation and evolution had remained largely unconstrained by observation. Following the Einstein X-ray Observatory surveys of supernova remnants and pulsars, however, strict temperature limits were placed on many putative neutron stars. The Einstein search for additional objects in the class of supernova remnants with embedded pulsars has increased the number of such objects by two. For the four objects in this class, the surface temperature limits (see Table 1) provide meaningful logically sound constraints on the neutron star models. For the future, however, still better X-ray observations are needed, both to increase the number of objects available for study and to refine the spatial and spectral capabilities of the X-ray measurements.

Rotational Properties of Neutron Star Models

Nature ◽  
1969 ◽  
Vol 224 (5219) ◽  
pp. 566-567 ◽  
Author(s):  
JEFFREY M. COHEN ◽  
A. G. W. CAMERON
Keyword(s):  
Neutron Star ◽  
Star Models

Neutron Star Matter and Neutron Star Models

1974 ◽  
Vol 29 (6) ◽  
pp. 933-946
Author(s):  
H. Heintzmann ◽  
W. Hillebrandt ◽  
M. F. El Eid ◽  
E. R. Hilf
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
High Mass ◽  
Mass Limit ◽  
Neutron Star Matter ◽  
Density Region ◽  
Star Models ◽  
Boson Exchange ◽  
Realistic Interaction ◽  
General Relativistic

Various methods to study the ground state of neutron star matter are compared and the corresponding neutron star models are contrasted with each other. In the low density region ρ < 1014gr cm-3 the nuclear gas is treated here by means of a Thomas Fermi method and the nuclei are described by the droplet model of Myers and Swiatecki. For ρ > 1014 gr cm-3 both standard Brueckner theory with more realistic interaction (one-boson-exchange) potentials and the semiphenomenological theory of Fermi liquids (together with the standard Reid softcore potential) are applied to neutron star matter. It is shown that while the high mass limit of neutron stars is hardly affected, some properties of lowmass neutron stars such as their binding depend sensitively on these refinements. Various tentative (but unreliable) extensions of the equation of state into high density regime ρ > 1015 gr cm-3 are investigated and it is shown that the mass limit for heavy neutron stars lies around 2.5 solar masses. It is further shown that a third family of stable (hyperon) stars is not forbidden by general relativistic arguments if there is a phase transition at high densities.

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