%0 Journal Article
%T New Solutions of Tolman-Oppenheimer-Volkov-Equation and of Kerr Spacetime with Matter and the Corresponding Star Models
%A Jan Helm
%J Journal of High Energy Physics, Gravitation and Cosmology
%P 724-767
%@ 2380-4335
%D 2022
%I Scientific Research Publishing
%R 10.4236/jhepgc.2022.83052
%X The Tolman-Oppenheimer-Volkov (TOV) equation is solved with a new ansatz: the external boundary condition with mass <i>M</i><sub>0</sub> and radius <i>R</i><sub>1</sub> is dual to the internal boundary condition with density <i>¦Ñ<sub>bc</sub></i> and inner radius <i>r</i><sub>i</sub>, and the two boundary conditions yield the same result. The inner boundary condition is imposed with a density <i>¦Ñ<sub>bc</sub></i> and an inner radius <i>r<sub>i</sub></i>, which is zero for the compact neutron stars, but non-zero for the shell-stars: stellar shell-star and galactic (supermassive) shell-star. Parametric solutions are calculated for neutron stars, stellar shell-stars, and galactic shell-stars. From the results, an M-R-relation and mass limits for these star models can be extracted. A new method is found for solving the Einstein equations for Kerr space-time with matter (extended Kerr space-time), <i>i.e.</i> rotating matter distribution in its own gravitational field. Then numerical solutions are calculated for several astrophysical models: white dwarf, neutron star, stellar shell-star, and galactic shell-star. The results are that shell-star star models closely resemble the behaviour of abstract black holes, including the Bekenstein-Hawking entropy, but have finite redshifts and escape velocity <i>v</i> < <i>c</i> and no singularity.
%K General Relativity
%K Tolman-Oppenheimer-Volkov Equation
%K Neutron Stars
%K Shell Stars
%U http://www.scirp.org/journal/PaperInformation.aspx?PaperID=118830