Fast and Slow Rotation of Asteroids

By P. Pravec, Alan W. Harris. 2000

387 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/89087163d07978c5a482af078690e1f948bb8f73

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

The strength of regolith and rubble pile asteroids (2013, background): “Small asteroids subject to the YORP effect experience a net torque due to solar photons interacting with the asymmetric surfaces of these bodies [34, 39].”
Equilibrium Configurations of Solid Cohesionless Bodies (2001, background): “Following the lead of Pravec and Harris (2000) , a list of near-Earth asteroids, Mars-crossers, and main belt asteroids was generated; Trojans and Centaurs were excluded.”
The Effect of Yarkovsky Thermal Forces on the Dynamical Evolution of Asteroids and Meteoroids (2002, background): “Mathematically similar derivations of this solution can be found in several modern references (Rubincam, 1995, 1998; Vokrouhlický, 1998a,b, 1999; Vokrouhlický and Farinella, 1999; Bottke et al., 2000a). In this chapter, we follow the formalism of Vokrouhlický (2001). Problem (1) above has already be”
Effects of thermal radiation on the dynamics of binary NEAs (2004, methodology): “Assuming an initial spin period of 3 h (Pravec and Harris, 2000), we compute τY 50,000 yr.”
LSST: From Science Drivers to Reference Design and Anticipated Data Products (2008, methodology): “…of asteroid families (Parker et al. 2008) and their correlations with age (Jedicke et al. 2004; Nesvorný et al. 2005); dynamical effects (Bottke et al. 2001); and studies of object shapes and spin states using light curve inversion techniques (Pravec & Harris 2000; Durech et al. 2009).”
Very low strengths of interplanetary meteoroids and small asteroids (2011, background): “…concluded on observational and theoretic grounds that many, if not most, kilometersized asteroids may have aggregate structure with low tensile strength; our work extends this concept down to decimeter sizes, though direct observations speak against aggregate structures (Pravec and Harris 2000).”
Full numerical simulations of catastrophic small body collisions (2008, background): “ision remnants are indistiguishable. 3.2. Strength Eects on Q D Small bodies in the solar system possess a wide range of shear strengths, from monolithic bodies inferred from fast spin rates, (e.g., Pravec and Harris 2000) to nearly strengthless bodies (e.g., ˘1 10 kPa for comet 9P/Tempel 1, Richard”
Bias-corrected population, size distribution, and impact hazard for the near-Earth objects (2004, background): “At about 200 m, asteroids probably change from being gravitationally bound rubble piles to being monoliths (Pravec and Harris, 2000; Whiteley et al., 2002).”
THE YARKOVSKY AND YORP EFFECTS: Implications for Asteroid Dynamics (2006, background): “Observation 4: The distribution of spin rates among observed small asteroids (D < 10 km) contains an excess number of fast rotators and very slow rotators when this data is fit to Maxwellian distribution (Pravec & Harris 2000, Pravec et al. 2002).”
A study of asteroid pole-latitude distribution based on an extended set of shape models derived by the lightcurve inversion method (2011, background): “It is known from previous studies (Pravec & Harris 2000; Rubincam 2000) that the YORP effect is significantly altering the periods and also spin vectors of these objects on a timescale shorter than the typical collisional lifetime of these objects (timescales are discussed in more details in Sect.”
YORP-induced long-term evolution of the spin state of small asteroids and meteoroids (2002, methodology): “Taking our estimates and 5 h for the typical rotation period of kilometer-sized asteroids (excluding slow rotators like Mathilde or Toutatis; see, e.g., Pravec and Harris 2001), we have a damping time scale of ≈45 Myr for the S-type and ≈5 Myr for the C-type asteroid of Rkm ≈ 1.”