| 1. | The major part of this perturbation is contributed by classical radiation pressure:
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| 2. | Over time, radiation pressure from the cluster will disperse the molecular cloud.
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| 3. | In the heaviest non-degenerate stars, radiation pressure is the dominant pressure component.
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| 4. | Solar radiation pressure affects bodies throughout much of the Solar System.
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| 5. | This is related to radiation pressure tangential to the grain's motion.
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| 6. | Both the lorentz force and radiation pressure only affect charged particles.
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| 7. | :You can read about this at Solar sail and radiation pressure.
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| 8. | This allows you to use conservation of momentum to calculate the radiation pressure.
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| 9. | :: According to solar sail, the pressure comes from radiation pressure.
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| 10. | :: : : There can be no radiation pressure without charges.
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