Particle falling radially into a black hole

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SUMMARY

The discussion centers on the Schwarzschild metric, which describes the spacetime geometry around a non-rotating black hole. The key equation presented details how a particle's proper time, denoted as ##\delta \tau##, changes as it moves in spherical coordinates from an initial position ##(r, \theta, \phi)## to a new position ##(r+\delta r, \theta + \delta \theta, \phi + \delta \phi)## over a time interval ##(t+\delta t)##. This equation incorporates gravitational effects through the terms involving the gravitational constant G, the speed of light c, and the radial coordinate r. Understanding this metric is essential for analyzing particle dynamics in the vicinity of black holes.

PREREQUISITES
  • Understanding of general relativity concepts
  • Familiarity with the Schwarzschild metric
  • Basic knowledge of spherical coordinates
  • Proficiency in calculus and differential equations
NEXT STEPS
  • Study the derivation of the Schwarzschild metric in detail
  • Explore the implications of the geodesic equation in curved spacetime
  • Learn about the effects of black hole gravity on time dilation
  • Investigate numerical simulations of particle trajectories near black holes
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Students of physics, particularly those studying general relativity, astrophysicists, and anyone interested in the dynamics of particles in strong gravitational fields.

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New poster has been reminded to show their work on schoolwork problems
Homework Statement
Attached it below
Relevant Equations
Not sure which equations necessary here.
I've been stuck starting anywhere with this. I need to finish this class for graduation and i'd like a safety net of a passing grade with this.
 

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Well, do you know what the Schwarzschild metric is? In Schwarzschild (spherical) coordinates, if a particle starts at the point ##r, \theta, \phi## at time ##t## and travels a small distance to the point ##r+\delta r, \theta + \delta \theta, \phi + \delta \phi## by time ##t+\delta t##, then the the change in proper time ##\delta \tau## satisfies:

##(\delta \tau)^2 = (1 - 2GM/(c^2 r))^{-1} (\delta t)^2 - (1 - 2GM/(c^2 r)) (\delta r)^2 - r^2 \delta \theta^2 - r^2 sin^2(\theta) (\delta \phi)^2##

You have to start with that as a "relevant equation".
 
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