Acceleration of the rotation of asteroid 1862 Apollo by radiation torques

  title={Acceleration of the rotation of asteroid 1862 Apollo by radiation torques},
  author={Mikko Kaasalainen and Josef Ďurech and Brian D. Warner and Yurij Krugly and Ninel M. Gaftonyuk},
The anisotropic reflection and thermal re-emission of sunlight from an asteroid’s surface acts as a propulsion engine. The net propulsion force (Yarkovsky effect) changes the orbital dynamics of the body at a rate that depends on its physical properties; for irregularly shaped bodies, the propulsion causes a net torque (the Yarkovsky–O'Keefe–Radzievskii–Paddack or YORP effect) that can change the object’s rotation period and the direction of its rotation axis. The Yarkovsky effect has been… 

The influence of global self-heating on the Yarkovsky and YORP effects

In addition to collisions and gravitational forces, there is a growing amount of evidence that photon recoil forces from the asymmetric reflection and thermal re-radiation of absorbed sunlight are

The strength and detectability of the YORP effect in near-Earth asteroids: a statistical approach

In addition to collisions and gravitational forces, it is now becoming widely acknowledged that photon recoil forces and torques from the asymmetric reflection and thermal re-radiation of sunlight

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The distribution of near‐Earth asteroid (NEA) rotation rates differs considerably from the similar distribution of Main Belt asteroids (MBAs) by the presence of excesses of fast and slow rotators,

Analysis of the rotation period of asteroids (1865) Cerberus, (2100) Ra-Shalom, and (3103) Eger - search for the YORP effect

Context. The spin state of small asteroids can change on a long timescale by the Yarkovsky-O’Keefe-Radzievskii-Paddack (YORP) effect, the net torque that arises from anisotropically scattered

Axial rotation of near-earth asteroids: The influence of the YORP effect

The distribution of axial rotation velocities of near-Earth asteroids (NEAs) substantially differs from that of the Main-Belt asteroids by an excess of both quickly and slowly rotating objects. Among

The Yarkovsky and YORP Effects

The Yarkovsky effect describes a small but significant force that affects the orbital motion of meteoroids and asteroids smaller than $30-40$ kilometers in diameter. It is caused by sunlight; when

The influence of rough surface thermal-infrared beaming on the Yarkovsky and YORP effects

It is now becoming widely accepted that photon recoil forces from the asymmetric reflection and thermal re-radiation of absorbed sunlight are, together with collisions and gravitational forces,

Detection of the YORP effect in asteroid (1620) Geographos

Aims. The rotation state of small asteroids is affected by the Yarkovsky-O’Keefe-Radzievskii-Paddack (YORP) torque. The directly observable consequence of the YORP effect is the secular change of the



Retrograde spins of near-Earth asteroids from the Yarkovsky effect

It is reported that the spin vectors of NEAs show a strong and statistically significant excess of retrograde rotations, quantitatively consistent with the theoretical expectations of the Yarkovsky model.

THE YARKOVSKY AND YORP EFFECTS: Implications for Asteroid Dynamics

The Yarkovsky and YORP (Yarkovsky-O’Keefe-Radzievskii-Paddack) effects are thermal radiation forces and torques that cause small objects to undergo semimajor axis drift and spin vector modifications,

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It is shown that thermal torques are more important than collisions in changing the spin states (and possibly shapes) of asteroids with diameters <40 km, and that in some cases, the asteroids become trapped in spin-orbit resonances.

Radiative Spin-up and Spin-down of Small Asteroids

The Yarkovsky–O'Keefe–Radzievskii–Paddack (YORP) effect may spin up or spin down 5-km-radius asteroids on a 108-year timescale. Smaller asteroids spin up or down even faster due to the radius-squared

Dynamical Spreading of Asteroid Families by the Yarkovsky Effect

Assuming that D ≲ 20 kilometer family members, since their formation, have undergone semimajor axis drift by the thermal force called the Yarkovsky effect helps explain why families are sharply bounded by nearby Kirkwood gaps, why some families have asymmetric shapes, and the curious presence of family members on short-lived orbits.