Density of asteroids

  title={Density of asteroids},
  author={Beno{\^i}t Carry},
  journal={Planetary and Space Science},
  • B. Carry
  • Published 20 March 2012
  • Geology, Physics
  • Planetary and Space Science

Figures and Tables from this paper

The Physical Properties and Composition of Main-Belt Asteroids from Infrared Spectroscopy
Asteroids are the remnants of planet formation, and as such, they represent a record of the physical and chemical conditions in the early solar system and its evolution over the past 4.6 billion
The origin of Phobos and Deimos is still an open question. Currently, none of the three proposed scenarios for their origin (intact capture of two distinct outer solar system small bodies,
Forming the Flora Family: Implications for the Near-Earth Asteroid Population and Large Terrestrial Planet Impactors
Formed from a catastrophic collision of a parent body larger than 150 km in diameter, the Flora family is located in the innermost part of the main belt near the secular resonance. Objects in this
The small binary asteroid ( 939 )
In understanding the composition and internal structure of asteroids, their density is perhaps the most diagnostic qua ntity. We aim here to characterize the surface composition, mutual orbit , size,
Multiple and fast: the accretion of ordinary chondrite parent bodies
Although petrologic, chemical, and isotopic studies of ordinary chondrites and meteorites in general have largely helped establish a chronology of the earliest events of planetesimal formation and
Metal Pollution of the Solar White Dwarf by Solar System Small Bodies
White dwarfs (WDs) often show metal lines in their spectra, indicating accretion of asteroidal material. Our Sun is to become a WD in several gigayears. Here, we examine how the solar WD accretes
Asteroids 87887 – 415992: the youngest known asteroid pair?
Context. Pairs of asteroids, that is, couples of single bodies on tightly similar heliocentric orbits, were recently postulated as a new category of objects in the solar system. They are believed to
Physical parameters of selected Gaia mass asteroids
Context. Thanks to the Gaia mission, it will be possible to determine the masses of approximately hundreds of large main belt asteroids with very good precision. We currently have diameter estimates


Binary asteroid population 1. Angular momentum content
Iron meteorites as remnants of planetesimals formed in the terrestrial planet region
It is shown that the iron-meteorite parent bodies most probably formed in the terrestrial planet region, and it is predicted that some asteroids are main-belt interlopers and a select few may even be remnants of the long-lost precursor material that formed the Earth.
Asteroids Were Born Big
Rotational breakup as the origin of small binary asteroids
It is found that mass shed from the equator of a critically spinning body accretes into a satellite if the material is collisionally dissipative and the primary maintains a low equatorial elongation.
The Gaia Mission: Expected Applications to Asteroid Science
According to current plans of the European space agency, Gaia will be launched in 2011. By performing a systematic survey of the whole sky down to magnitude V = 20, this mission will provide a
Contamination of the asteroid belt by primordial trans-Neptunian objects
It is shown that the violent dynamical evolution of the giant-planet orbits required by the so-called Nice model leads to the insertion of primitive trans-Neptunian objects into the outer belt, implying that the observed diversity of the asteroid belt is not a direct reflection of the intrinsic compositional variation of the proto-planetary disk.
The techniques described in an earlier paper were used to determine masses of 104 asteroids by the method of asteroid–asteroid gravitational interaction. For each of the 104 perturbers, 4 large sets
From the Cradle to the Grave: The Rise and Demise of the Comets
In this chapter, we discuss the processes that drive the physical transformation and decay of cometary nuclei as they move from the frigid outer regions into the hot environment of the inner solar