CONICET | Buscador de Institutos y Recursos Humanos

This article is continuation of previous papers [1,7], where we have been discussed the radial pulsations of strongly collapsed strange stars. To explore the structure and oscillatory behaviour of dense nuclear matter we study of the oscillationg motion of massive collapsed stars, which comprise compact objects like neutron stars [4], [8] and [10], and the strange stars [5]. To analyse the rotational and oscillating dynamics of ordinary stars from the main sequence, the Kelvin hydrodynamic model of the stellar continuum is often used [2]. In this approach the dynamics of stellar matter is described by equations of a self-gravitating non-viscous incompressible liquid. The current investigations of macroscopic properties of atomic nuclei show that an oscillating heavy nucleus behaves like a piece of elastic solid rather than like a liquid [6]. In view of this, we see the importance to examine the hydrodynamic approach and to develop the elastodynamic method for the investigation of the structure and oscillating dynamics of nuclear stellar objects. While the assumption of uniformly distributed matter inside a neutron star does not reflect the real stratified structure inferred from evolution calculations [10], the homogeneous model allows one to elucidate in analytic form the difference in the oscillating dynamics of collapsed star presumedly possessing elastodynamic and hydrodynamic properties of nuclear stellar matter.