Authors: DT Froedge
In previous papers we have discussed the concept of a theory of gravitation with local energy conservation, and the properties of a large neutron star resulting when the energy of gravitation resides locally with the particle mass and not in the gravitational field [1][2][3]. A large neutron star’s surface radius grows closer to the gravitational radius as the mass increases, but is always slightly larger. As the mass increases there is a continuously greater mass defect for incoming particles. Since the localization of energy applies to the photon, a photon does not decrease in energy rising in a gravitational field, and can thus escape. Photon trajectories in a strong gravitational field have some peculiar features that are not immediately obvious, but can be investigated by the use of ray tracing procedures. The most notable is the fact that only a fraction of the blackbody radiation emitted from the surface escapes into space (about 0.00004% for Sag A*). The remainder enters orbit below the maximum photon orbit. Because of the low percent of escaping blackbody radiation, the heavy neutron stars considered in this paper will be referred to as a Neutron Dark Star (NDS). In contrast to the Black Hole (BH) which should be totally dark inside the photon shadow, the NDS will appear as a fuzzy low luminosity ball with a Full Width Half Maximum intensity diameter of about 3.85 Schwarzschild radii inside the shadow. This paper will investigate the difference in the appearance of a Neutron Dark Star and a Black Hole by using ray tracing techniques. The Event Horizon Telescope currently under development should be able to distinguish the difference between the theories.
Comments: 25 Pages. Presented APS Baltimore APRil 2015
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[v1] 2014-07-01 13:41:13
[v2] 2014-11-19 15:36:33
[v3] 2015-04-18 10:05:48
[v4] 2016-06-21 18:42:11
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