THE SPHERICALLY SYMMETRIC BODY IN RELATIVISTIC ELASTICITY

2012 ◽  
Author(s):  
J. FRAUENDIENER
Keyword(s):  
Symmetric Body ◽  
Spherically Symmetric

Spherically Symmetric Vibration of an Elastic Spherical Shell Subject to a Radial and Time-Dependent Body-Force Field

1971 ◽  
Vol 38 (3) ◽  
pp. 702-705 ◽  
Author(s):  
J. M. McKinney
Keyword(s):  
Continuous Function ◽  
Spherical Shell ◽  
Force Field ◽  
Body Force ◽  
Time Dependent ◽  
Symmetric Body ◽  
Spherically Symmetric ◽  
Symmetric Vibration ◽  
Elastic Spherical Shell

A solution, exact within the framework of linear elastokinetics, is obtained for a vibrating, elastic, arbitrarily thick spherical shell subject only to a spherically symmetric body force field of the form FR(r, τ) = Fr(r)Ft(τ). Fr(r) is taken in the form of a polynomial whereas Ft(τ) is restricted only to being a sectionally continuous function of time.

scholarly journals Absence of Singularity in Schwarzschild Metric in the Vector Model for Gravitational Field

2012 ◽  
Vol 18 (3) ◽  
pp. 175-184
Author(s):  
Vo Van On
Keyword(s):  
Black Hole ◽  
Gravitational Field ◽  
General Theory ◽  
Space Time ◽  
Symmetric Body ◽  
Vector Model ◽  
Spherically Symmetric ◽  
Theory Of Relativity ◽  
General Theory Of Relativity ◽  
Schwarzschild Metric

In this paper, based on the vector model for gravitational field we deduce an equation to determinate the metric of space-time. This equation is similar to equation of Einstein. The metric of space-time outside a static spherically symmetric body is also determined. It gives a small supplementation to the Schwarzschild metric in General theory of relativity but the singularity does not exist. Especially, this model predicts the existence of a new universal body after a black hole.

scholarly journals Stability Against Radial Perturbations of Slowly Rotating Neutron Stars

1981 ◽  
Vol 93 ◽  
pp. 327-327
Author(s):  
Kenzo Arai ◽  
Keisuke Kaminishi
Keyword(s):  
General Relativity ◽  
Equation Of State ◽  
Angular Velocity ◽  
Neutron Stars ◽  
Radial Displacement ◽  
Cold Neutron ◽  
Symmetric Body ◽  
Slow Rotation ◽  
Spherically Symmetric ◽  
Dynamical Equations

The dynamical equations governing pulsation in rotating neutron stars are derived in the framework of general relativity. Stellar models are constructed by using a realistic equation of state for cold neutron matter. Small radial displacement and slow rotation are treated as perturbations on spherically symmetric body. In these models the maximum masses are 1.761 M⊙ at the central density 3.461 × 1015 g cm−3 for a sequence of nonrotating configurations and 2.165 M⊙ for rotating models with the critical angular velocity (GM/R3)½.

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