Volume 598, February 2017
|Number of page(s)||13|
|Section||Planets and planetary systems|
|Published online||31 January 2017|
Escape of asteroids from the main belt
1 Department of Physics, PO Box 64, 00014 University of Helsinki, Finland
2 Observatoire de la Côte d’Azur, Boulevard de l’Observatoire, 06304, Nice Cedex 4, France
3 Institute for Astronomy, Charles University, V Holešovičkách 2, 18000 Prague 8, Czech Republic
4 Southwest Research Institute, 1050 Walnut St., Ste. 300, Boulder, CO 80302, USA
5 Institute for Astronomy, University of Hawaii, 2680 Woodlawn Dr., 96822 Honolulu, HI, USA
Received: 5 July 2016
Accepted: 4 November 2016
Aims. We locate escape routes from the main asteroid belt, particularly into the near-Earth-object (NEO) region, and estimate the relative fluxes for different escape routes as a function of object size under the influence of the Yarkovsky semimajor-axis drift.
Methods. We integrated the orbits of 78 355 known and 14 094 cloned main-belt objects and Cybele and Hilda asteroids (hereafter collectively called MBOs) for 100 Myr and recorded the characteristics of the escaping objects. The selected sample of MBOs with perihelion distance q > 1.3 au and semimajor axis a < 4.1 au is essentially complete, with an absolute magnitude limit ranging from HV < 15.9 in the inner belt (a < 2.5 au) to HV < 14.4 in the outer belt (2.5 au < a < 4.1 au). We modeled the semimajor-axis drift caused by the Yarkovsky force and assigned four different sizes (diameters of 0.1, 0.3, 1.0, and 3.0 km) and random spin obliquities (either 0 deg or 180 deg) for each test asteroid.
Results. We find more than ten obvious escape routes from the asteroid belt to the NEO region, and they typically coincide with low-order mean-motion resonances with Jupiter and secular resonances. The locations of the escape routes are independent of the semimajor-axis drift rate and thus are also independent of the asteroid diameter. The locations of the escape routes are likewise unaffected when we added a model for Yarkovsky-O’Keefe-Radzievskii-Paddack (YORP) cycles coupled with secular evolution of the rotation pole as a result of the solar gravitational torque. A Yarkovsky-only model predicts a flux of asteroids entering the NEO region that is too high compared to the observationally constrained flux, and the discrepancy grows larger for smaller asteroids. A combined Yarkovsky and YORP model predicts a flux of small NEOs that is approximately a factor of 5 too low compared to an observationally constrained estimate. This suggests that the characteristic timescale of the YORP cycle is longer than our canonical YORP model predicts.
Key words: minor planets, asteroids: general / methods: numerical / methods: statistical / surveys / celestial mechanics / planets and satellites: dynamical evolution and stability
© ESO, 2017
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