Editing YORP effect (section)

{{Short description|Second-order variation on the Yarkovsky effect that changes rotation rates of small bodies}}
{{distinguish|Yarkovsky effect}}The '''Yarkovsky–O'Keefe–Radzievskii–Paddack effect''', or '''YORP effect''' for short, changes the rotation state of a small [[astronomical body]] – that is, the body's [[rotation period|spin rate]] and the [[Axial tilt|obliquity]] of its [[Poles of astronomical bodies|pole]](s) – due to the [[scattering]] of [[solar radiation]] off its surface and the [[Emission (electromagnetic radiation)|emission]] of its own [[thermal radiation]].

The YORP effect is typically considered for [[asteroid]]s with their [[heliocentric orbit]] in the [[Solar System]]. The effect is responsible for the creation of [[Binary asteroid|binary]] and [[tumbling asteroids]] as well as for changing an asteroid's pole towards 0[[Degree (angle)|°]], 90°, or 180° relative to the [[ecliptic plane]] and so modifying its heliocentric radial drift rate due to the [[Yarkovsky effect]].