The Yarkovsky effect is a phenomenon that causes force to act on a rotating celestial body, such as an asteroid, due to the way it absorbs and re-emits sunlight as heat. The Yarkovsky effect depends on many physical and surface properties of the body such as diameter, albedo, density, obliquity, and rotation period.
The visual magnitude V of an asteroid is a measure of how bright it appears to an observer.
Heliocentric distance r is the distance between the object and the sun's center.
H is the absolute magnitude of the asteroid,
Delta is range to the observer (in au),
g(t) is a periodic function related to the asteroid shape in rotation, it is used to describe the repeating brightness variations (light curve) of an asteroid over time.
The phase function describes how brightness evolves with the phase angle(the Sun-asteroid-observer angle). The phase function is second-degree polynomial here.
To find g(t), fourier series has been used upto 10 order here.
If the shape of an asteroid is well-described by a tri-axial ellipsoid, the light-curve is expected to display two local maxima and two local minima. local maxima and local minima are the peaks and troughs of the asteroid's brightness variations over time.
Source: https://arxiv.org/abs/2501.07189
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