A Hamiltonian formulation of relativistic fluid dynamics in curved spacetime in coordinate time is proposed and applied to Schwarzschild radial flows, but the derived equations and stability conclusion are not fully supported.
Pseudo-Schwarzschild Description of Accretion-Powered Spherical Outflow
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Using two different pseudo-Schwarzschild potentials proposed by Artemova et. al,$^{1}$ we formulate and solve the equations governing spherically symmetric transonic inflow and outflow in presence of a relativistic hadronic pressure mediated steady, standing, spherical shock around the central compact object and then we self-consistently connect the accretion-wind solutions to calculate the mass outflow rate $R_{\dot m}$ in terms of minimum number of flow parameters. Also we study the dependence of this rate on various boundary conditions governing the flow.
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Relativistic Fluid Dynamics in Curved Spacetime: a Novel Effective Hamiltonian Approach
A Hamiltonian formulation of relativistic fluid dynamics in curved spacetime in coordinate time is proposed and applied to Schwarzschild radial flows, but the derived equations and stability conclusion are not fully supported.