Yarkovsky Effect on Small Near-Earth Asteroids: Mathematical Formulation and Examples

By David Vokrouhlický, Andrea Milani, S. Chesley. 2000

171 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/d764cdfed518b713e1da0526e31209ae9594c51a

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Citations in the corpus

THE YARKOVSKY AND YORP EFFECTS: Implications for Asteroid Dynamics (2006, methodology): “They found that the nongravitational acceleration experienced on Golevka was consistent with the Yarkovsky theory (e.g., Vokrouhlický et al. 2000, 2001b), with their best-fit values yielding a bulk density of 2.7 ± 0.2 g cm−3 and K ∼ 0.01 W m−1 K−1.”
Predicting the Earth encounters of (99942) Apophis (2008, methodology): “The equations of motion were extended to specify these six models, according to Vokrouhlický et al. (2000), using a linearized heat diffusion computational subroutine provided by Vokrouhlický and Chesley.”
The YORP effect with finite thermal conductivity (2004, background): “Both Golevka and 1998 KY26 were predicte be good candidates for detection of the Yarkovsky ef (Vokrouhlický et al., 2000), and in the Golevka’s case th detection has been already achieved(Chesley et al., 2003).”
Near Earth Asteroids with measurable Yarkovsky effect (2012, background): “Typical values of da/dt for sub-kilometer NEAs are 10–10 au/Myr (Vokrouhlický et al., 2000).”
YORP-induced long-term evolution of the spin state of small asteroids and meteoroids (2002, background): “…and Vokrouhlický 1999, Bottke et al. 2001a), processes in the asteroid families (e.g., Vokrouhlický et al. 2001, Nesvorný et al. 2002, Bottke et al. 2001b), or the possibility of directly detecting the Yarkovsky orbital perturbations of the near-Earth asteroids (e.g., Vokrouhlický et al. 2000).”
Orbit and bulk density of the OSIRIS-REx target Asteroid (101955) Bennu (2014, methodology): “The linear model utilizes linearized heat transfer equations on a rotating homogeneous sphere, closely following the development given by Vokrouhlický et al. (2000) for both the diurnal and seasonal components of the Yarkovsky effect.”
Asteroid family ages (2015, methodology): “Although other methods are possible, currently the most precise method to constrain the age of a collisional family (for the ages older than ∼ 10 My) exploits non-gravitational perturbations, mostly the Yarkovsky effect (Vokrouhlický et al., 2000).”
The Effect of Yarkovsky Thermal Forces on the Dynamical Evolution of Asteroids and Meteoroids (2002, methodology): “If the modeling work of Vokrouhlický et al. (2000) is correct, radar observations during the next close encounters of the most promising candidate asteroids may produce a discernable Yarkovsky “footprint.””
Irradiation Records, Cosmic-Ray Exposure Ages, and Transfer Times of Meteorites (2006, background): “Consideration of the Yarkovsky effect seems to resolve several problems (Farinella et al., 1998; Vokrouhlicky et al., 2000; Spitale and Greenberg, 2002).”