Binary asteroid population 1. Angular momentum content
By P. Pravec, Alan W. Harris. 2007
261 citations recorded by the source corpus.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/9f210cc4b29f42ea8bd76d810d2e578c571d57b7
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
- William Bottke
- David Vokrouhlický
- Federica Spoto
- Andrea Milani
- F. DeMeo
- Benoît Carry
- Seth Andrew Jacobson
- Daniel J. Scheeres
Citations in the corpus
- Near Earth Asteroids with measurable Yarkovsky effect (2012, methodology): “…D we used either the known value when available or an assumed value computed from the absolute magnitude H according to the following relationship (Pravec and Harris, 2007): D = 1329 km × 10 −0.2H √ pV (12) where pV is the albedo, assumed to be 0.154 if unknown, in agreement with the Palermo…”
- The taxonomic distribution of asteroids from multi-filter all-sky photometric surveys (2013, methodology): “ons by volume and mass). 7.2. Asteroid distribution by surface area To estimate the surface area of each asteroid, we need first to estimate its diameter D. For that we use the following equation from Pravec and Harris (2007, and references therein): D = 1329 p a 10 0:2 H (3) where H is the absolute ”
- Absolute magnitudes of asteroids and a revision of asteroid albedo estimates from WISE thermal observations (2012, unknown): “The relationship between the effective diameter, geometric albedo, and absolute magnitude is where (See Pravec and Harris, 2007, for its derivation from the definition of those parameters plus the apparent magnitude of the Sun at 1 AU, V Sun , which includes the definition of the V magnitude scale.)”
- Dynamics of rotationally fissioned asteroids: Source of observed small asteroid systems (2011, methodology): “They also have high mass ratios & 0.2 and a system semi-major axis of 2 to 8 primary diameters (Pravec and Harris, 2007).”
- The strength of regolith and rubble pile asteroids (2013, background): “rvations of small asteroid spins and morphologies. The cumulative work and cataloging represented by Pravec, Harris and collaborators has been captured in the small body rotation and binary databases [41, 24]. The most signicant results were the initial publication of the size/spin rate plots in [23”
- Density of asteroids (2012, methodology): “From the absolute magnitude H and an assumed geometric albedo p , the diameter is given by f ð km Þ ¼ 1329 p (cid:2) 0 : 5 10 (cid:2) 0 : 2 H (Pravec and Harris, 2007, and references therein).”