1994/02/03 by Xingming Chen, Ronald E. Taam · 1 citation
Engineering · Physics and Astronomy · #Accretion (finance) #Astrophysical Phenomena and Observations #Astrophysics #Black hole (networking) #Mechanics and Biomechanics Studies #Neutron star #Physics #Quantum mechanics #Quasi periodic #Viscosity #astro-ph
paper · pdf · doi:10.1086/174524
18 Pgs, LaTex; 9 Figs available upon request. To Appear in ApJ
arxiv created 1994/02/03 · openalex publication_date 1994/08/01 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We consider the inner regions of accretion disks surrounding black holes and neutron stars and investigate the nonlinear time dependent evolution of thermal-viscous instabilities. The viscous stress is assumed to be proportional to the gas pressure with the viscosity parameter formulated as α =min[α0 (h/r)n, αmax], where h is the local scale height, r is the distance from the central compact object, and n, α0 and αmax are constants. It is found that the disk is unstable for α sufficiently sensitive to h (n \gapprox 1.2). The instabilities are globally coherent in the entire unstable region of the disk and, depending on the viscosity parameters, the time variability of the mass accretion rates are manifested as periodic or quasi-periodic oscillations. We show that, the low frequency (∼ 0.04~Hz) quasi-periodic oscillations (QPOs) discovered recently in some of the black hole candidates (Cyg~X-1 and GRO~J0422+32) and a low mass X-ray binary (Rapid Burster MXB~1730--335) may be explicable by the thermal-viscous instabilities in accretion disks. The observations of QPOs place constraints on the viscosity parameters and suggest that (n,α0) ∼ (1.6,30) for the Rapid Burster with a 1.4 \msun neutron star. In the case of black hole candidates, the dependence of α on h/r is less steep corresponding to n ∼ 1.2-1.3 for black holes less than 10 \msun.