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A Population of Comets in the Main Asteroid Belt
Science, 2006Comets are icy bodies that sublimate and become active when close to the Sun. They are believed to originate in two cold reservoirs beyond the orbit of Neptune: the Kuiper Belt (equilibrium temperatures of ∼40 kelvin) and the Oort Cloud (∼10 kelvin).
David Jewitt, Henry H. Hsieh
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On the asteroid belt's orbital and size distribution
Icarus, 2009Abstract For absolute magnitudes greater than the current completeness limit of H-magnitude ∼15 the main asteroid belt's size distribution is imperfectly known. We have acquired good-quality orbital and absolute H-magnitude determinations for a sample of small main-belt asteroids in order to study the orbital and size distribution beyond H = 15
Gladman, Brett +11 more
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1996
In 1772, Johann Titius, a German astronomer, came to Johann Bode at the Berlin Observatory with a simple mathematical relationship he had discovered that appeared to give the orbits of the planets. He pointed out that if you start with the series 0, 3, 6, 12, 24,..., add four to each, then divide by 10 you get the distance to each of the planets in ...
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In 1772, Johann Titius, a German astronomer, came to Johann Bode at the Berlin Observatory with a simple mathematical relationship he had discovered that appeared to give the orbits of the planets. He pointed out that if you start with the series 0, 3, 6, 12, 24,..., add four to each, then divide by 10 you get the distance to each of the planets in ...
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Some peculiarities in the Asteroidal Belt
Earth, Moon, and Planets, 1986The analysis of the fine structure of the Asteroidal Belt evidenciates a group of asteroids next to the resonance 4/9 with Jupiter. In this group and in other groups associated to the Hirayama families there are indications that their orbital parameters can be represented by quantum numbers as defined here and in two of our previous works.
R. J. Quiroga, Ricardo R. Cordeiro
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Structure and evolution of the asteroid belt
International Astronomical Union Colloquium, 1974AbstractInvestigations concerning the structure of the asteroid belt make it possible to distinguish four main stages in its evolution. The first stage. The formation of a certain number of protoplanets (ten-hundred) between the orbits of Mars and Jupiter, simultaneously with major planets.
M. Ia. Shmakova, G. A. Chebotarev
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Resonant structure of the asteroid belt
Nature, 1981Statistical techniques are applied to asteroid orbital data in an attempt to define the characteristics of the Kirkwood gaps in the distribution of the asteroids. A significant tendency is found for the eccentricities and inclinations of asteroid orbits to increase away from the gaps.
Carl D. Murray, Stanley F. Dermott
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Resonances and chaos in the asteroid belt
International Astronomical Union Colloquium, 1999AbstractThe present paper reviews the evolution of our understanding of the effect of resonances on the distribution of asteroids in the asteroid belt. The history of this problem goes back to the Kirkwood's discovery (1867) of the Kirkwood gaps located at resonances with Jupiter.
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Mass distribution in the asteroid belt
Earth, Moon, and Planets, 1992The dependence of the cumulative number of numbered asteroids (up to 3720) on their absolute magnitude is investigated. The differential mass index k is derived from these relations for fainter asteroids. A steeper slope (2.2 < k < 2.4) is found in the four most populous asteroid familes (Flora, Koronis, Eos and Themis) and a flatter slope (1.3 < k < 1.
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A note on the cosmogony of the asteroidal belt
Astrophysics and Space Science, 1976Several arguments based on the orbital dynamics of the asteroids are used to support the idea that the original solar nebula might not necessarily be the Laplacian type of thin disk-like structure. The orbital distribution of the large asteroids is suggested to be a direct result of their accretions of condensed grains in eccentric orbits via the jet ...
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On the Amount of Dust in the Asteroid Belt
International Astronomical Union Colloquium, 1971Calculations of upper limits to the quantity of small particles in the asteroid belt are based on (1) the brightness of the counterglow coupled with observations and theory for the zodiacal cloud near Earth's orbit and (2) the destruction and erosion of asteroidal particles as they spiral toward the Sun because of solar radiation via the Poynting ...
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