2009/11/12 by Bernd Aschenbach, Bernd Eduard Aschenbach, Aschenbach, Bernd Eduard
Engineering · Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics of Galaxies (astro-ph.GA) #FOS: Physical sciences #Mechanics and Biomechanics Studies #Pulsars and Gravitational Waves Research #astro-ph.GA
paper · pdf · doi:10.48550/arxiv.0911.2431
revised version of a paper presented at the 2009 Frascati Workshop, Vulcano, May 2009, to be published in Mem.S.A.It
arxiv created 2009/11/12 · openalex publication_date 2009/11/12 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
The analysis of flare start-times confirms the periods found years ago (Aschenbach et al., 2004) in the near-infrared and X-ray light-curves related to the Sgr A* black hole. The assignment of the frequencies found to radial and vertical epicyclic frequencies ν\sb\rm r, ν\sb\rm v, respectively, as well as to the Kepler orbital frequency ν\sb\rm K reveals resonances of ν\sb\rm v / ν\sb\rm r=7:2, and ν\sb\rm K / ν\sb\rm v=3:1. The highest observed frequency of 10 mHz is identified as the Kepler frequency corrected by the rotational frame-dragging frequency, as expected from the Lense-Thirring effect. These frequency assignments conclude a black hole mass of M = (4.10-4.34)×10\sp6 M_\odot and a spin of a = (0.99473-0.99561).