2D Phase portrait - Black hole?

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SUMMARY

The discussion focuses on analyzing trajectories around a black hole using the equation ## \frac{d^2u}{d\theta^2} + u = \alpha \epsilon u^2 ##, where ##u = \frac{1}{r}##. In part (a), the system is reduced to 2D, identifying fixed points at ##(0,0)## and ##(\frac{1}{\epsilon}, 0)##, with the former being a center and the latter a saddle point based on eigenvalue analysis. Part (b) explores the stability of these fixed points, concluding that for ##|u| > \frac{1}{2\epsilon}##, particles do not get trapped by the black hole.

PREREQUISITES
  • Understanding of differential equations and stability analysis
  • Familiarity with phase portraits in dynamical systems
  • Knowledge of eigenvalues and eigenvectors
  • Basic concepts of black hole physics and gravitational dynamics
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  • Explore the implications of non-linear dynamics in black hole physics
  • Learn about perturbation theory in celestial mechanics
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Physicists, mathematicians, and students studying dynamical systems, particularly those interested in gravitational physics and the behavior of trajectories in the vicinity of black holes.

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Homework Statement



Trajectories around a black hole can be described by ## \frac{d^2u}{d\theta^2} + u = \alpha \epsilon u^2 ##, where ##u = \frac{1}{r}## and ##\theta## is azimuthal angle.

(a) By using ##v = \frac{du}{d\theta}##, reduce system to 2D and find fixed points and their stability. Find direction of fastest perturbations.
(b) Sketch the phase portrait. Would stability of fixed points differ in the non-linearized version?

Homework Equations

The Attempt at a Solution



Part (a)
The equations now become ##\delta v = \delta \dot u## and ##\delta \dot v + \delta u = 2\epsilon u \delta u##.
2010_B1_Q1.png

Fixed points are ##\left( 0,0 \right)## and ##\left( \frac{1}{\epsilon}, 0 \right)##. At ##(0,0)##, all eigenvalues are imaginary, so the fixed point is a center. At ##(\frac{1}{\epsilon},0)##, eigenvalues are ##\pm 1## so fixed point is a saddle.
Eigenvalue of ##J + J^T## is ##2\epsilon u## and direction of fastest perturbation is ##u=v##.

Part(b)
Eigenvalue in general is ##\lambda^2 = (2\epsilon u - 1)##, so for ##|u| > \frac{1}{2\epsilon}##, the particle doesn't get trapped by the black hole?

2010_B1_Q1_2.png

 
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