Radiation Pressure and Solar Sail

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SUMMARY

The discussion focuses on calculating the required area of a solar sail to propel a spacecraft with a mass of 1000 kg away from the Sun. The key formula derived is based on the relationship between pressure, force, and momentum, specifically using the equation F = GMm/r² and the concept of luminosity as energy per unit time. The participant emphasizes the need to understand the solar constant, which represents the intensity of solar radiation at Earth's orbit, to accurately compute the necessary sail area. The discussion highlights the importance of relating energy, momentum, and gravitational forces in the context of solar sailing.

PREREQUISITES
  • Understanding of gravitational force calculations (F = GMm/r²)
  • Knowledge of momentum and pressure relationships in physics
  • Familiarity with solar luminosity and the solar constant
  • Basic principles of impulse and energy transfer (E = p*c)
NEXT STEPS
  • Research the solar constant and its value at Earth's orbit
  • Learn about the physics of solar sails and their design considerations
  • Explore the calculations involved in momentum transfer from radiation pressure
  • Study gravitational interactions in space travel and propulsion methods
USEFUL FOR

Aerospace engineers, physicists, and students interested in space propulsion technologies, particularly those focusing on solar sailing and gravitational dynamics.

jmm5872
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Consider a spacecraft attached to a sheet of material, a "sail," that absorbs sunlight. Assume that the sail is positioned to face the Sun and that the combined mass of the spacecraft and the sail is m. How large does the area of the sail have to be to propel the spacecraft away from the Sun? m = 1000 kg.

My thoughts on how to figure this out...

Calculate the momentum per unit area per unit time of the radiation leaving the Sun, which seems to me to be the pressure by this relation:

Pressure = Force/Area = momentum/(area*time)

Then find the force that arises from the pressure on the solar sail, and this needs to oppose the gravitational force of the Sun.

I think it is this: F = GMm/r2 = Ut/c
where momentum p = U/c, and it's derivative is F = Ut/c

And U is energy coming from the Sun. This is more of my confusion. I know Luminosity is energy per unit time, I just don't really know how to use all of this to get what I need. I think I am just missing some of the conceptual part that would help me relate everything and simply plug in the given mass.
 
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I think of it via the impulse formula F*Δt = change in momentum
For light, E = p*c so p = E/c and F = (E/Δt)/c = Intensity*Area/c.
The question doesn't say what distance from the sun. Earth orbit would be convenient; there the intensity is called the solar constant and it can be looked up in Wikipedia.
 

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