2012/05/29 by Robert V. Wagoner
Earth and Planetary Sciences · Physics and Astronomy · #Accretion (finance) #Accretion disc #Angular momentum #Astrophysical Phenomena and Observations #Astrophysics #Binary number #Black hole (networking) #Classical mechanics #Geometry #High-pressure geophysics and materials #Line (geometry) #Mode (computer interface) #Oscillation (cell signaling) #Physics #Pulsars and Gravitational Waves Research #Quasi periodic #Spin (aerodynamics) #astro-ph.HE #gr-qc
paper · pdf · doi:10.1088/2041-8205/752/2/l18
published as Ap.J. 752, L18 (2012) · Accepted for publication in Astrophysical Journal Letters; 9 pages, references added and typos corrected
openalex publication_date 2012/05/29 · arxiv created 2012/06/01 · arxiv updated 2012/06/04 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We compare the determinations of the angular momentum of stellar mass black holes via the continuum and line methods with those from diskoseismology. The assumption that is being tested is that one of the quasi-periodic oscillations (QPOs) in each binary X-ray source is produced by the fundamental g -mode. This should be the most robust and visible normal mode of oscillation of the accretion disk, and therefore its absence should rule out diskoseismology as the origin of QPOs. The comparisons are consistent with the second highest frequency QPO being produced by this g -mode, but are not consistent with models in which one QPO frequency is that of the innermost stable circular orbit.