Expansion and rotational momentum of large cosmic masses.
Abstract
A 'large cosmic mass' is defined as a system of particles with given mass and a gravitational radius somewhat larger than its 'baryon radius'. If such a mass is extremely dense and forms a system resembling a neutron superstar, it will collapse completely within its Schwarzschild radius and become the center of a black hole. The stability of a homogeneous large cosmic mass with initial nuclear density is considered from the viewpoint of geometrodynamics, allowing for the possibility of 'gravity absorption' or an increase in effective inertial mass due to induction of inertia by a local gravitational potential. It is shown that such a mass may have equilibrium configurations and should expand when equilibrium is disrupted. Analysis in the framework of various cosmological models indicates that a specific asymptotic relation between mass and moment of rotation will be obeyed during such expansion. It is concluded that the present mathematical model of a radially expanding system of large mass with initial nuclear density provides a simple dynamic description of Ambartsumian's (1972) hypothesis that galaxies and clusters of galaxies originated from dense giant nuclei.
 Publication:

Astrofizika
 Pub Date:
 August 1976
 Bibcode:
 1976Afz....12..511T
 Keywords:

 Astrophysics;
 Cosmology;
 Rotating Bodies;
 Stellar Rotation;
 Asymptotic Methods;
 Black Holes (Astronomy);
 Expansion;
 Galactic Clusters;
 Mathematical Models;
 Neutron Stars;
 Astrophysics