Calculating Black Particle Size in a Red Giant Solar System - Astronomy Homework

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SUMMARY

The discussion focuses on calculating the critical size of black spherical particles in a red giant solar system, specifically when the Sun's brightness increases by a factor of 5000 and its mass decreases to half. The key equations involve the balance of radiation force and gravitational force, represented as F=((flux)*π a^2 Q)/c and GMm/r^2. Participants clarify that 'a' represents the particle radius, 'Q' denotes the energy received, and 'flux' is the light intensity. The solution requires understanding the gravitational force on a particle, the light force on an area, and the mass and cross-sectional area of a sphere.

PREREQUISITES
  • Understanding of gravitational force equations (GMm/r^2)
  • Knowledge of radiation pressure and flux calculations
  • Familiarity with spherical geometry and density calculations
  • Basic principles of astrophysics related to stellar evolution
NEXT STEPS
  • Research the concept of radiation pressure and its effects on small particles
  • Study the derivation of gravitational force equations in astrophysical contexts
  • Learn about the properties of blackbody radiation and energy absorption
  • Explore the implications of stellar evolution on planetary systems
USEFUL FOR

Astronomy students, astrophysicists, and anyone interested in the dynamics of particle behavior in stellar environments, particularly during the red giant phase of stars.

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Homework Statement


When the Sun becomes a red giant star its brightness will increase by a factor of 5000 and its mass will decrease to half of its present mass. When this happens particles smaller than a critical size will be blown out (light force = gravity force) of the solar system by the pressure of sunlight. What is the size for a black spherical particles ( they absorb all light that falls on them) with density of 1000 kg/m^3.

Homework Equations



radiation force on a spherical particle=F=((flux)*π a^2 Q)/c

The Attempt at a Solution



So in the problem it says that the light force = grav force
((flux)*π a^2 Q)/c = GMm/r^2 = GM/r^2 * (4π a^3 ρ)/3
(from example in book)
But I don't know what a, Q or flux is. I would estimate r= 1AU.
This also wouldn't use the change in brightness.
Need some help on where to go with this problem because I think I'm setting this up all wrong :(
 
Last edited:
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Since the attractive gravitational force and the amount of light hitting the particle both drop off as r^2 they cancel - the effect is the same at any distance.

a looks like the radius of the particle.
Q is normally the energy received.

You need an equation for
1, the attractive force of gravity on a particle of mass m
2, the force of light on an area A
3, the equation for the mass and cross section area of a sphere of a given radius and density.
Then you just set equations 1 and 2 equal.
 

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