
The mechanical force exerted by light on surfaces it strikes, used here to synchronize vibrations.Radiation pressure is the mechanical force exerted by light or other electromagnetic radiation on a surface it strikes. Although light has no mass, it carries momentum, and when photons are absorbed or reflected, they transfer that momentum to the object. This pressure is minuscule in everyday life—sunlight exerts about 9 micronewtons per square meter—but it becomes significant in precision physics and space technology.
The concept was first proposed by Johannes Kepler in 1619 to explain why comet tails point away from the Sun, and was later derived from Maxwell's electromagnetic theory in the 19th century.
When a photon hits a surface, its momentum is transferred. If the surface is reflective, the photon bounces back, transferring twice the momentum compared to absorption. The cumulative effect of many photons produces a steady force. In optomechanics, this force can be used to cool or synchronize the vibrations of tiny mechanical resonators, effectively coupling light and motion.
Radiation pressure is used to manipulate microscopic objects in optical tweezers, to stabilize the orientation of spacecraft via solar sails, and to cool mechanical resonators in quantum experiments.
A solar sail the size of a football field would experience about 0.01 newtons of force from sunlight—enough to slowly accelerate a spacecraft over months.



