scholarly journals General Relativistic Effects on Neutrino‐driven Winds from Young, Hot Neutron Stars andr‐Process Nucleosynthesis

2000 ◽  
Vol 533 (1) ◽  
pp. 424-439 ◽  
Author(s):  
Kaori Otsuki ◽  
Hideyuki Tagoshi ◽  
Toshitaka Kajino ◽  
Shin‐ya Wanajo
Keyword(s):  
Neutron Stars ◽  
Relativistic Effects ◽  
General Relativistic

scholarly journals Types of Stellar Instabilities

1980 ◽  
Vol 5 ◽  
pp. 433-436
Author(s):  
P. Ledoux
Keyword(s):  
Neutron Stars ◽  
Linear Theory ◽  
White Dwarfs ◽  
Relativistic Effects ◽  
Significant Information ◽  
Average Value ◽  
Eigen Values ◽  
Late Evolution ◽  
General Relativistic ◽  
Formation Phase

Aside from violent phenomena, regular forms of motions originate often in instabilities and the linear theory with terms ∞ exp (st) yields already significant information. The system, here a spherical star, will be the seat of an instability if R (s) > 0. In general, s will be complex as both conservative (adiabatic) and non-conservative (non-adiabatic) factors are present. However if the latter (small) are neglected, the eigen-values s2 often denoted -σ2 are real. If at least one σ2 < 0, then the star is dynamically unstable.Radial perturbations. If an appropriate average value Γ1 > 4/3, then all σ2 are positive. If Γ < 4/3 (formation phase: ionization; late evolution: nuclear equilibrium; degeneracy in white dwarfs and neutron stars or radiation in very large masses plus general relativistic effects) the fundamental eigenvalue of only becomes negative.

scholarly journals General Relativistic Theory of Rotating Neutron Stars – A Review

1971 ◽  
Vol 46 ◽  
pp. 334-340
Author(s):  
Jeffrey M. Cohen
Keyword(s):  
General Relativity ◽  
Neutron Stars ◽  
Relativistic Theory ◽  
White Dwarfs ◽  
Relativistic Effects ◽  
Red Shift ◽  
Light Bending ◽  
Perihelion Advance ◽  
General Relativistic

Except in cosmology, astrophysicists are used to thinking of general relativistic effects as small (e.g., light bending, perihelion advance, red shift) and have generally left such problems to general relativists. However, the discovery of pulsars (Hewish et al., 1968) may have changed this. Not only is general relativity necessary to treat rotating neutron stars, but relativity was also partly responsible for the elimination of pulsating white dwarfs as pulsar models.

Beyond the Schwarzschild Metric

2018 ◽  
Author(s):  
David M. Wittman
Keyword(s):  
Black Holes ◽  
General Relativity ◽  
Gravitational Waves ◽  
Test Particle ◽  
Direct Detection ◽  
Relativistic Effects ◽  
Big Bang ◽  
Clusters Of Galaxies ◽  
General Relativistic ◽  
The Universe

General relativity explains much more than the spacetime around static spherical masses.We briefly assess general relativity in the larger context of physical theories, then explore various general relativistic effects that have no Newtonian analog. First, source massmotion gives rise to gravitomagnetic effects on test particles.These effects also depend on the velocity of the test particle, which has substantial implications for orbits around black holes to be further explored in Chapter 20. Second, any changes in the sourcemass ripple outward as gravitational waves, and we tell the century‐long story from the prediction of gravitational waves to their first direct detection in 2015. Third, the deflection of light by galaxies and clusters of galaxies allows us to map the amount and distribution of mass in the universe in astonishing detail. Finally, general relativity enables modeling the universe as a whole, and we explore the resulting Big Bang cosmology.

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