# Generalized Newtonian description of particle motion in spherically symmetric spacetimes

@article{Tejeda2014GeneralizedND, title={Generalized Newtonian description of particle motion in spherically symmetric spacetimes}, author={Emilio Tejeda and Stephan Rosswog}, journal={arXiv: General Relativity and Quantum Cosmology}, year={2014} }

We present a generalized Newtonian description of particle dynamics valid for any spherically symmetric, static black hole spacetime. This approach is derived from the geodesic motion of test particles in the low-energy limit. It reproduces exactly the location of the marginally stable, marginally bound, and photon circular orbits; the radial dependence of the energy and angular momentum of circular orbits; parabolic motion; pericentre shift; and the spatial projection of general trajectories…

## 7 Citations

### Pseudo-Newtonian Equations for Evolution of Particles and Fluids in Stationary Space-times

- Physics
- 2016

Pseudo-Newtonian potentials are a tool often used in theoretical astrophysics to capture some key features of a black hole space-time in a Newtonian framework. As a result, one can use Newtonian…

### Accretion onto deformed black holes via pseudo–Newtonian potentials

- PhysicsProceedings of High Energy Astrophysics in Southern Africa — PoS(HEASA2018)
- 2019

The Johannsen-Psaltis spacetime describes a rotating black hole with parametric deviations from the Kerr metric. By construction this spacetime explicitly violates the no-hair theorems. Rotating…

### Bondi accretion in the spherically symmetric Johannsen–Psaltis spacetime

- PhysicsThe European Physical Journal C
- 2019

The Johannsen–Psaltis spacetime explicitly violates the no-hair theorem. It describes rotating black holes with scalar hair in the form of parametric deviations from the Kerr metric. In principle,…

### Unsettling Physics in the Quantum-Corrected Schwarzschild Black Hole

- PhysicsSymmetry
- 2020

This unsettling physics, which deviates radically from both Schwarzschild (near the horizon) and Minkowski (at infinity) is due to repulsion by the negative quantum energy density that makes the quasilocal mass vanish as one approaches spatial infinity.

### Free Motion around Black Holes with Disks or Rings: Between Integrability and Chaos–V

- PhysicsThe Astrophysical Journal
- 2019

The complete integrability of geodesic motion, the well-known feature of fields of isolated stationary black holes, can easily be “spoiled” by the presence of some additional sources (even if highly…

### Orbit classification in an equal-mass non-spinning binary black hole pseudo-Newtonian system

- Physics
- 2018

The dynamics of a test particle in a non-spinning binary black hole system of equal masses is numerically investigated. The binary system is modeled in the context of the pseudo-Newtonian circular…

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