scholarly journals Observational Constraints on the Surface Gravitational Redshift of a Neutron Star

2017 ◽  
Author(s):  
Masachika Iwai ◽  
Tadayasu Dotani ◽  
Masanobu Ozaki ◽  
Yoshitomo Maeda ◽  
Hideyuki Mori ◽  
...  
Keyword(s):  
Neutron Star ◽  
Gravitational Redshift ◽  
Observational Constraints

scholarly journals Neutron star cooling: theoretical aspects and observational constraints

2004 ◽  
Vol 33 (4) ◽  
pp. 523-530 ◽  
Author(s):  
D.G Yakovlev ◽  
O.Y Gnedin ◽  
A.D Kaminker ◽  
K.P Levenfish ◽  
A.Y Potekhin
Keyword(s):  
Neutron Star ◽  
Observational Constraints ◽  
Neutron Star Cooling

scholarly journals Double dark matter admixed neutron star

2018 ◽  
Vol 27 (16) ◽  
pp. 1950002 ◽  
Author(s):  
Zeinab Rezaei
Keyword(s):  
Dark Matter ◽  
Neutron Star ◽  
Equation Of State ◽  
Neutron Stars ◽  
Equations Of State ◽  
Compact Object ◽  
Gravitational Redshift ◽  
Two Fluid

The dark matter (DM) in neutron stars can exist from the lifetime of the progenitor or when captured by this compact object. The properties of DM that enter the neutron stars through each step could be different from each other. Here, we investigate the structure of neutron stars which are influenced by the DM in two processes. Applying a generalization of two-fluid formalism to three-fluid one and the equation-of-state from the rotational curves of galaxies, we explore the structure of double DM admixed neutron stars. The behavior of the neutron and DM portions for these stars is considered. In addition, the influence of the DM equations of state on the stars with different contributions of visible and DM are studied. The gravitational redshift of these stars in different cases of DM equations of state is investigated.

scholarly journals X-Ray Bursts of Nuclear Origin?

1977 ◽  
Vol 4 (1) ◽  
pp. 127-128 ◽  
Author(s):  
L. Maraschi ◽  
A. Cavaliere
Keyword(s):  
Neutron Star ◽  
Nuclear Energy ◽  
Observational Constraints ◽  
X Ray ◽  
Thermonuclear Reactions ◽  
Cold Star ◽  
Pycnonuclear Reactions

The fate of nuclear energy carried by matter accreted onto a neutron star was considered e.g. by Rosenbluth et al. (1973). They examined pycnonuclear reactions on an originally cold star, and found that the whole star is thereby heated up to 106−107 °K. The thermonuclear reactions that can be ignited then, have been studied by Hansen and Van Horn (1975), who computed stationary burning shells, finding, however, that in most cases the shells are thermally unstable.We consider here the possibility that X-ray bursts are due to instabilities of this type. The observational constraints fix the parameters uniquely.

scholarly journals Electron capture reactions in neutron star crusts: deep heating and observational constraints

2010 ◽  
Author(s):  
Edward Brown ◽  
Sanjib S. Gupta ◽  
Hendrik Schatz ◽  
Peter Möller ◽  
Karl Ludwig Kratz
Keyword(s):  
Neutron Star ◽  
Electron Capture ◽  
Observational Constraints

scholarly journals About Bonnor Solution and Gravitational Redshift

2017 ◽  
Vol 45 ◽  
pp. 1760048
Author(s):  
Orlenys Troconis ◽  
Viviane Alfradique ◽  
Rodrigo Negreiros
Keyword(s):  
Dipole Moment ◽  
Neutron Star ◽  
Magnetic Fields ◽  
Magnetic Dipole ◽  
Maxwell Equations ◽  
Magnetic Dipole Moment ◽  
Polar Angle ◽  
Gravitational Redshift ◽  
Schwarzschild Solution ◽  
Emission Signal

We consider the analytical Bonnor solution for a relativistic neutron star and discuss about the limit in which this solution satisfies Einstein-Maxwell equations. We study the gravitational redshift for Bonnor solution without electric charge. We find that for stars with magnetic fields up to [Formula: see text] in the center, the gravitational redshift for Bonnor metric differs from the Schwarzschild solution on a term that depends on magnetic dipole moment and the polar angle of the emission signal.

Towards the extreme

2019 ◽  
pp. 250-281
Author(s):  
Nils Andersson
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
First Principles ◽  
Observational Constraints ◽  
Simple Matter ◽  
Matter Model ◽  
The Impact

The main aspects of neutron star physics are discussed, including the problem of determing the equation of state from first principles (using a simple matter model as example). Available observational constraints on mass and radius are considered. The effect of rotation is considered and the impact of superfluidity (manifesting itself in terms of pulsar glitches) is discussed.

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