Abstract Details

Name: Prerna Rana
Affiliation: Indian Institute of Astrophysics
Conference ID: ASI2021_438
Title : A geometric origin for temporal properties of black hole systems
Authors and Co-Authors : Prerna Rana (Indian Institute of Astrophysics, Bangalore-560034), Arun Mangalam (Indian Institute of Astrophysics, Bangalore-560034)
Abstract Type : Oral
Abstract Category : Stars, ISM and Galaxy
Abstract : We present a generalized relativistic precession model (GRPM) which associates the fundamental frequencies of the non-equatorial (with Carter's constant, $Q\neq 0$) and eccentric ($e\neq 0$) particle trajectories around a Kerr black hole with the frequencies of Quasi-periodic oscillations (QPOs) observed in the X-ray light curves of black hole X-ray binaries (BHXRBs) and active galactic nuclei (AGN). We study cases of BHXRB M82 X-1, GROJ 1655-40, XTEJ 1550-564, 4U 1630-47, and GRS 1915+105, and extract the parameters \{$e$, $r_p$, $a$, $Q$\}, where $r_p$ is the periastron distance of the orbit, and $a$ is the spin of the black hole. We find that the non-equatorial eccentric solutions for QPOs, when taken together, span a torus region and give rise to a strong QPO signal. We also show that the eccentric orbit solution fits the PBK correlation. Our analysis of the fluid flow in the relativistic disk edge suggests that instabilities cause QPOs to originate in a torus. We also find that the 3:2 ratio of high-frequency QPOs observed in BHXRBs corresponds to a single leaf zoom-whirl 3D periodic orbit with two azimuthal whirls. We also apply the GRPM to QPOs observed in the Narrow-line Seyfert 1 galaxies 1H 0707-945, REJ 1034+396, 2XMM J123103.2+110648, MS 2254.9-3712, Mrk 766, and MCG-06-30-15. The origin of these QPOs is attributed to the plasma motion in the corona region. By applying the lighthouse model, we propose a kinematic origin of the jet based $\gamma$-ray and optical QPOs, in a relativistic MHD framework. We also present the relativistic orbit model (ROM) for Fourier power spectral density (PSD) shape observed in certain AGN and we show that PSD has a break corresponding to the energy at ISCO.