Why the astrophysical black hole candidates are not rotating black holes

It is believed that the basic component of the central engine of quasars, microquasars, and energetic Gamma Ray Bursts are the rotating or the Kerr Black Holes (BH)[1]. But by using a generic property[2-4] of the metric components of a stationary axisymmertic rotating metric in its standard form, namely, gφφ = sin 2 θgθθ, where φ is the azimuth angle and θ is the polar angle measured from the axis of symmetry, we have found the unexpected and surprising result that (i) in order to have a mass of a Kerr BH m ≥ 0, it is necessary that its rotation parameter a = 0 and if one insists for an a ≥ 0, one must have m ≤ 0! Thus if the suspected Black Hole candidates with m > 0 are really rotating they cannot be BHs at all which is in agreement with some detailed analysis of recent observations[5-8]. However, if it is assumed that such objects are strictly non-rotating, they could be non-rotating Schwarzschild BHs (a = 0) with m ≥ 0 if we ignore the physical difficulties associated with the existence of such objects. This result calls for new theoretical efforts to understand a vast range of astrophysical phenomenon. If one derives the Kerr Metric in a straightforward manner by using the Backlund transformation, it is seen that a = m sinφ. This relationship confirms that a = m = 0 for Kerr BHs. To describe the axially symmetric stationary Kerr spacetime or any other axially symmetric stationary spacetime, it is convenient to consider x = t, the time coordinate, and x = φ, the azimuth angle. By definition, for such a spacetime, the metric coefficients are independent of t and φ: