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