Origin of Multikilometer Earth- and Mars-Crossing Asteroids: A Quantitative Simulation-Reference-Cited by-同舟云学术

Origin of Multikilometer Earth- and Mars-Crossing Asteroids: A Quantitative Simulation

Published:1998-09-25 Issue:5385 Volume:281 Page:2022-2024
ISSN:0036-8075
Container-title:Science
language:en
Short-container-title:Science

Author:

Migliorini Fabio¹,Michel Patrick¹,Morbidelli Alessandro¹,Nesvorný David¹,Zappalà Vincenzo¹

Affiliation:

1. F. Migliorini, Armagh Observatory, College Hill BT61 9DG, Northern Ireland, United Kingdom, and Osservatorio Astronomico di Torino, I-10025 Pino Torinese, Italy. P. Michel, Osservatorio Astronomico di Torino, I-10025 Pino Torinese, Italy, and Observatoire de la Côte d'Azur, B.P. 4229, 06304 Nice cedex 4, France. A. Morbidelli and D. Nesvorný, Observatoire de la Côte d'Azur, B.P. 4229, 06304 Nice cedex 4, France. V. Zappalà, Osservatorio Astronomico di Torino, I-10025 Pino Torinese, Italy.

Abstract

Orbital dynamic simulations show that many asteroids in the main asteroid belt are driven toward Mars-crossing orbits by numerous weak mean motion resonances, which slowly increase the orbital ellipticity of the asteroids. In addition, half of the Mars-crossing asteroids (MCAs) transition to Earth-crossing asteroids (ECAs) in less than 20 million years. This scenario quantitatively explains the observed number of large ECAs and MCAs.

Publisher

American Association for the Advancement of Science (AAAS)

Subject

Multidisciplinary

Reference25 articles.

1. See for instance R. Greenberg and M. Nolan in Asteroids II R. Binzel T. Gerhels M. S. Matthews Eds. (Univ. of Arizona Press Tucson AZ 1989) pp. 778–804.

2. Mainly the 3/1 mean motion resonance with Jupiter which occurs when the orbital period of the asteroid is equal to 1/3 the Jovian period or the ν 6 secular resonance which occurs when the mean precession rate of the asteroid's perihelion equals that of Saturn. These are by far the most efficient resonances for the transport of bodies to large eccentricities.

3. For a list of ECAs and MCAs with perihelion distance < 1.3 AU (classically defined as Amors asteroids) see .

4. Dynamical Lifetimes of Objects Injected into Asteroid Belt Resonances

5. Here ECAs are defined as the asteroids with perihelion and aphelion distance smaller and larger respectively than 1 AU whereas MCAs are defined as those that are not currently Earth crossers and intersect the orbit of Mars within one precession cycle of their orbit. To identify all MCAs we have integrated for 300 000 years the evolution of all the asteroids in the 1997 update of the catalog [E. Bowell K. Muinonen L. H. Wasserman in Asteroids Comets Meteors A. Milani M. DiMartino A. Cellino Eds. (Kluwer Dordrecht Netherlands 1994) pp. 477–481] with perihelion distance smaller than 1.78 AU. An asteroid has been categorized as MCA if it passes through the torus defined by heliocentric distance r between 1.341 and 1.706 AU and vertical coordinate | z | < r sin(6.4°). These bounds account for a martian maximal eccentricity and inclination of 0.12 and 6.4° respectively. Asteroid diameters have been estimated assuming the albedos reported in Table 1 if IRAS measurements are not available.

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