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Long-term evolution of asteroids in the 2:1 Mean Motion Resonance

Published online by Cambridge University Press:  05 January 2015

Despoina K. Skoulidou ,
Kleomenis Tsiganis  and
Harry Varvoglis
Despoina K. Skoulidou
Affiliation:
Section of Astrophysics, Astronomy & Mechanics, Department of Physics, Aristotle University of Thessaloniki, 54 124 Thessaloniki, Greece email: dskoulid@physics.auth.gr, tsiganis@auth.gr, varvogli@physics.auth.gr
Kleomenis Tsiganis
Affiliation:
Section of Astrophysics, Astronomy & Mechanics, Department of Physics, Aristotle University of Thessaloniki, 54 124 Thessaloniki, Greece email: dskoulid@physics.auth.gr, tsiganis@auth.gr, varvogli@physics.auth.gr
Harry Varvoglis
Affiliation:
Section of Astrophysics, Astronomy & Mechanics, Department of Physics, Aristotle University of Thessaloniki, 54 124 Thessaloniki, Greece email: dskoulid@physics.auth.gr, tsiganis@auth.gr, varvogli@physics.auth.gr
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Abstract

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The problem of the origin of asteroids residing in the Jovian first-order mean motion resonances is still open. Is the observed population survivors of a much larger population formed in the resonance in primordial times? Here, we study the evolution of 182 long-lived asteroids in the 2:1 Mean Motion Resonance, identified in Brož & Vokrouhlické (2008). We numerically integrate their trajectories in two different dynamical models of the solar system: (a) accounting for the gravitational effects of the four giant planets (i.e. 4-pl) and (b) adding the terrestrial planets from Venus to Mars (i.e. 7-pl). We also include an approximate treatment of the Yarkovksy effect (as in Tsiganis et al.2003), assuming appropriate values for the asteroid diameters.

Keywords

asteroidsmethods: numericalresonancesYarkovsky effect
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Issue S310: Complex Planetary Systems , July 2014 , pp. 178 - 179
Copyright
Copyright © International Astronomical Union 2014 

References

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