2004/09/02 by Abhas Mitra, Mitra, Abhas
Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics (astro-ph) #Astrophysics and Cosmic Phenomena #FOS: Physical sciences #Pulsars and Gravitational Waves Research #Relativity and Gravitational Theory
paper · pdf · doi:10.48550/arxiv.astro-ph/0409049
openalex publication_date 2004/09/02 · openalex created_date 2022/09/30 · openalex updated_date 2026/07/28
In a recent paper[1], it has been shown that, there cannot be any rotating\n(Kerr) Black Hole (BH) with finite mass in order that the generic properties\nassociated with the symmetries of stationary axisymmetric Einstein equations\nare obeyed, i.e, in order to have m\≥ 0, we must have a=0. In other words,\nall observed chargeless BHs with finite masses must be non-rotating\nSchwarzschild BHs. Here, by comparing the invariant 4 volume associated with\noriginal Kerr metric [2] with the Boyer-Lindquist version of the same [3], we\nfurther find that, stationary axisymmetric em vacuum Einstein solutions\nactually correspond to m=0 in addition to a=0! This means that if the Kerr\nsolution is a unique one, the Schwarzschild BHs too correspond to only m=0 and\ntherefore the observed BH candidates (BHs) with m >0 are not BHs at all. This\nis in agreement some detailed analysis of recent observations[4-7] which\nsuggest the the BHCs have strong intrinsic magnetic moment rather than any\nEvent Horizon. If one would derive the Boyer-Lindquist metric in a\nstraightforward manner by using the Backlund transformation, it would follow\nthat a= m sin phi, where phi is the azimuth angle. This relationship directly\nconfirms the result that for a supposed rotating BH, actually, both a=m=0.\n