Abstract

The compact black hole primary in the X-ray binary Cygnus X-1, has recently been characterised by observation. This data can be analysed to test models of black hole gravitational physics. Using the optimum observational data with the least fit parameters, the average of 3 spectral data sets revealed an averaged inner rim accretion disc radius R_in = 2.24 GM/c². Using the Kerr spinning black hole model results in a theoretical apparent reduction in R_in = 1.41 GM/c², which also results in an extremely relativistic spin parameter a_* > 0.97 c. Here the data is analysed using a dynamic gravitational model. Utilizing this model R_in = 2.24 GM/c², which is equivalent to the observed R_in = 2.24 GM/c². In this case the spin parameter does not reach such extreme relativistic speeds, at a_* = 0.76 c. These results using dynamic black hole physics are in very good agreement with direct observations of Cygnus X-1. Importantly, this model offers further testable predictions of black hole gravitational physics.

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