Distinguishing a Kerr-like black hole and a naked singularity in perfect fluid dark matter via precession frequencies

Abstract

We study a Kerr-like black hole and naked singularity in perfect fluid dark matter (PFDM). The critical value of spin parameter a c is presented to differentiate the black hole from naked singularity. It is seen that for any fixed value of dark matter parameter α the rotating object is black hole if a ≤ a c and naked singularity if a > a c . Also for −2 ≤ α < 2/3 the size of the black hole horizons decrease whereas for 2/3 < α it increases. We also study spin precession frequency of a test gyroscope attached to stationary observer to differentiate a black hole from naked singularity in PFDM. For the black hole, spin precession frequency blows up as the observer reaches the central object while for naked singularity it remains finite except at the ring singularity. Moreover, we study Lense-Thirring precession for a Kerr-like black hole and geodetic precession for Schwarzschild black hole in PFDM. To this end, we have calculated the Kepler frequency (KF), the vertical epicyclic frequency (VEF), and the nodal plane precession frequency (NPPF). Our results show that, the PFDM parameter α significantly affects those frequencies. This difference can be used by astrophysical observations in the near future to shed some light on the nature of dark matter.

Testing the weak cosmic censorship conjecture for a Reissner–Nordström–de Sitter black hole surrounded by perfect fluid dark matter

“…Dark matter has not been so far detected directly, yet astrophysical observations indicate that many giant elliptical and spiral galaxies contain a (sometimes a binary) supermassive black hole in the galactic center embedded in a giant dark matter halo [3,4,[65][66][67][68]. In the literature, several black hole solutions with a dark matter background have been proposed (see for example [69][70][71][72][73][74][75][76][77][78]). The analysis of the accretion process for different spherically symmetric spacetime geometries for a static fluid and the accretion of phantom energy onto a stationary charged black hole has been investigated testing under various conditions (see for example [79,80]).…”

Epicyclic Oscillations around Simpson-Visser Regular Black Holes and Wormholes

“…Of course, in making definite conclusions, some additional phenomena have to be considered such as the precession frequencies of some orbiting mass [53] and the optical phenomena such as shadow [54,55].…”

X-ray reflection spectroscopy with Kaluza–Klein black holes

“…The gravitational field of the BH causes the rotational axis of a gyroscope to precess, and the precession frequency carries unique signatures of the BH metric. Such precession frequencies have been calculated in several non-Kerr spacetimes [31][32][33][34].…”