Direct Evidence Of Gravitational Waves Surrounding the Sgr A* Supermassive Black Hole and an Estimation of Mass

Details Direct Evidence Of Gravitational Waves Surrounding the Sgr A* Supermassive Black Hole and an Estimation of Mass Direct Evidence Of Gravitational Waves Surrounding the Sgr A* Supermassive Black Hole and an Estimation of Mass

Sep 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aas...206.4603d&link_type=abstract

American Astronomical Society Meeting 206, #46.03; Bulletin of the American Astronomical Society, Vol. 37, p.792

Astronomy and Astrophysics

Astronomy

Scientific paper

Normal modes of vibration [``The Mathematical Theory of Black Holes and of Colliding Plane Waves", Chandrasekhar 1991; Ferrari in "Black Holes and Relativistic Stars", Wald 1998] of the supermassive black hole (SBH) at the galactic center (GC) produce resonant quasi-stationary (long-lived) gravitational waves in the region close to the event horizon. In turn, these waves couple to non-zero mass electrons that travel through the same region, causing these particles to oscillate at the normal mode frequencies and emit electromagnetic radiation at the resonant frequencies. A peak intensity is emitted from electrons at distances around 1.5 RS where RS is the radius of the event horizon. We show that the black hole spin angular momentum has only a small influence upon the frequencies of these normal modes.
Evidence that these low-frequency vibrations are occurring is established by matching these frequencies with a subset of the Quasi-Periodic Oscillations (QPOs) in the amplitudes of the infrared and x-ray power spectra. Solutions to the General Relativistic wave equation near the SBH show that these frequencies depend inversely upon the mass of the SBH, allowing the mass to be determined by the respective QPO frequencies.
This method of determining the mass of the SBH at GC, is based upon electron behavior close to the event horizon rather than behavior of stellar objects at much greater distances from the SBH. The value of the mass is repeatedly and consistently obtained from each of several QPOs in each of the available experimental energy bands (IR and X-ray) which correspond to gravitational wave natural modes. The available experimental power spectra have only been reported at discrete values of frequency, causing most of the uncertainty in our SBH mass estimate.

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