| 41. | The eccentricity ( i . e . the eccentricity vector ) is perturbed by the solar radiation pressure.
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| 42. | This helps stabilize the disk against radiation pressure which would otherwise blow the material away into interstellar space.
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| 43. | What prevents that from happening is the radiation pressure of all of the light coming from the star.
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| 44. | At this point the internal radiation pressure is sufficient to slow the inward collapse almost to a standstill.
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| 45. | This wave is coupled with the spatial variation of the bubble density under the action of radiation pressure forces.
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| 46. | Another but equivalent way to interpret the principle of optomechanical cavities is by using the concept of radiation pressure.
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| 47. | Radiation pressure from the star will push the dust particles away into interstellar space over a relatively short timescale.
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| 48. | The radiation pressure results in forces and torques on the bodies that can change their translational and rotational motions.
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| 49. | Solar sails rely on radiation pressure from electromagnetic energy, but they require a large collection surface to function effectively.
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| 50. | This reduction in gamma ray energy density reduces the radiation pressure that supports the outer layers of the star.
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