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| Yarkovsky effect | |
|---|---|
| Name | Yarkovsky effect |
| Phenomenon | Thermal recoil force on rotating bodies in space |
| Discovered | Early 20th century |
| Discoverer | Ivan Osipovich Yarkovsky |
| Field | Astrodynamics, Celestial mechanics, Planetary science |
Yarkovsky effect The Yarkovsky effect is a subtle nongravitational perturbation on the orbits of small Solar System bodies produced by anisotropic thermal emission from a rotating surface. It influences the long-term orbital evolution of asteroids, meteorite delivery, and the dynamical pathways connecting populations such as the main asteroid belt, near-Earth object, and Jupiter-family comet reservoirs.
The effect operates on meter- to kilometer-scale bodies including meteoroids, asteroids, and artificial satellite debris, producing semimajor axis drift that competes with gravitational perturbations from Jupiter, Saturn, Earth, and resonances such as the 3:1 Kirkwood gap, ν6 secular resonance, and mean-motion resonances. It contributes to the supply of near-Earth asteroids to the inner Solar System and affects populations studied by missions like NEOWISE, Hayabusa2, OSIRIS-REx, and surveys including Pan-STARRS, Catalina Sky Survey, and Vera C. Rubin Observatory. The effect is relevant to interpretation of meteorite fall statistics associated with families such as Flora family, Eunomia family, and Vesta family.
Thermal photons carry momentum; when a rotating body absorbs sunlight from Sun and re-emits infrared radiation, anisotropy in the timing and direction of emission produces a net force. The diurnal component depends on rotation state (prograde or retrograde spin) relative to orbit and is modulated by thermal inertia, surface conductivity, and albedo characteristics tied to materials like olivine, pyroxene, and carbonaceous matter found on C-type asteroid, S-type asteroid, and D-type asteroid surfaces. The seasonal component depends on obliquity and orbital motion, interacting with tidal torques from bodies such as Moon and close encounters with planets like Mars or Venus. Surface roughness and regolith properties studied at Ryugu and Bennu alter emission patterns; laboratory experiments at institutions like Jet Propulsion Laboratory, European Space Agency, and Max Planck Institute for Solar System Research inform thermophysical parameters.
Analytical and numerical models express acceleration as a function of thermal recoil proportional to irradiance, emissivity, and temperature gradients. Seminal formulations build on radiation force theory used in Poynting–Robertson effect analyses and incorporate heat conduction solutions from the one-dimensional heat equation with boundary conditions anchored to rotation period and solar incidence. Yarkovsky force components are often decomposed into transverse, radial, and normal terms within the framework of Gauss's planetary equations and integrated with N-body codes such as Mercury, REBOUND, and specialized thermophysical models developed by teams at University of Pisa, University of Arizona, and University of Bern. Parameter estimation employs techniques like Bayesian inference, Markov chain Monte Carlo, and covariance analysis used in orbit determination at Jet Propulsion Laboratory, Minor Planet Center, and European Southern Observatory.
Direct detections derive from precise astrometry combining optical observations from facilities such as Hubble Space Telescope, Very Large Telescope, Subaru Telescope, and radar ranging from Goldstone Deep Space Communications Complex and Arecibo Observatory prior to its collapse. Notable measurements include semimajor axis drift for (6489) Golevka, (101955) Bennu, and (1862) Apollo inferred from decades-long datasets contributed by International Astronomical Union, Minor Planet Center, and survey programs. Thermal-infrared measurements by Spitzer Space Telescope, WISE, and AKARI constrain surface properties that feed into models validated against shape models from missions like NEAR Shoemaker, Hayabusa, and OSIRIS-REx.
Over Myr to Gyr timescales, Yarkovsky-driven drift moves bodies across resonances, reshaping size-frequency distributions in the main belt and creating dynamical links to near-Earth objects, Trojan asteroids, and Hungaria family. It contributes to the dispersal of collisional families such as Karin cluster and Veritas family and explains age-dependent dispersion patterns used in chronology by researchers at Southwest Research Institute, NASA, and CNRS. Interactions with non-gravitational effects like YORP effect spin-up, collisions cataloged by AIDA studies, and chaotic diffusion in resonance zones produce complex evolutionary pathways modeled by teams at Caltech, Cornell University, and MIT.
Accurate assessment of impact probabilities for hazardous asteroids such as (101955) Bennu and (99942) Apophis requires inclusion of Yarkovsky accelerations in orbit propagation and risk corridors computed by agencies including NASA, ESA, JAXA, and national space agencies. Deflection strategies considered in concepts like kinetic impactor tests, gravity tractor proposals, and mission designs (e.g., DART, HERA) must account for long-term Yarkovsky-modified trajectories and post-mitigation thermal responses. Planetary defense pipelines at Jet Propulsion Laboratory and European Space Agency integrate thermophysical uncertainty into impact probability calculations communicated through Minor Planet Center notices.
The principle traceable to early ideas on thermal forces was proposed by Ivan Yarkovsky in unpublished notes and later resurrected and elaborated by Ernst J. Öpik and Radzievskii (astronomer) in the mid-20th century. Modern quantitative treatment emerged in work by Peter Goldreich, Stanley F. Dermott, and later by researchers such as Vokrouhlický, Bottke, and teams at University of Pisa and Charles University in Prague who connected theory to asteroid family observations. Instrumental advances from observatories like Palomar Observatory and space telescopes enabled empirical detections in the late 20th and early 21st centuries.
Related nongravitational processes include the YORP effect, Poynting–Robertson effect, and thermal recoil forces on artificial satellites relevant to missions operated by NASA, ESA, and commercial entities like SpaceX. Applications extend to asteroid family dating, meteorite source identification linking to H chondrites and HED meteorites, and spacecraft navigation strategies for missions to small bodies where thermal forces can be exploited for trajectory control tested in missions such as Hayabusa2 and OSIRIS-REx.
Category:Celestial mechanicsCategory:Asteroids