Hot Spots in Sgr A* Accretion Disk: Hydrodynamic Insights

Abstract

The recent image of our galaxy’s supermassive black hole Sgr A* derived from the 7 April 2017 data of the Event Horizon Telescope Collaboration shows multiple hot spots in its accretion disk. Using the analytical framework, we demonstrate that the observed hot spots may not be disjoint elements but causally linked components (“petals”) of one rotating quasi-stationary macro-structure formed in the thermo-vorticial field within the accretion disk.

Dynamics of Vortex Structures: From Planets to Black Hole Accretion Disks

“…For a strongly localized vortex-see, for example, Ref. [17]-quantity q(x, t) can be parameterized by a function in the form F(x − x 0 (t)), i.e., the one with the center at coordinate x = x 0 (t), which satisfies the equation of transport ẋ0k (t) + ϵ ik ∂ i ψ = 0. In other words, in such cases, the center of the vortex moves according to ẋ0 (t) − v[x 0 (t)] = 0.…”