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Impactor Flux on the Pluto-Charon System

Published online by Cambridge University Press:  06 April 2010

Gonzalo C. de Elía ,
Romina P. Di Sisto  and
Adrián Brunini
Gonzalo C. de Elía
Affiliation:
Facultad de Ciencias Astronómicas y Geofísicas - UNLP, IALP - CCT La Plata - CONICET, Paseo del Bosque S/N (1900), La Plata, Buenos Aires, Argentina email: [email protected], [email protected], [email protected]
Romina P. Di Sisto
Affiliation:
Facultad de Ciencias Astronómicas y Geofísicas - UNLP, IALP - CCT La Plata - CONICET, Paseo del Bosque S/N (1900), La Plata, Buenos Aires, Argentina email: [email protected], [email protected], [email protected]
Adrián Brunini
Affiliation:
Facultad de Ciencias Astronómicas y Geofísicas - UNLP, IALP - CCT La Plata - CONICET, Paseo del Bosque S/N (1900), La Plata, Buenos Aires, Argentina email: [email protected], [email protected], [email protected]
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Abstract

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In this work, we study the impactor flux on Pluto and Charon due to the collisional evolution of Plutinos.To do this, we develop a statistical code that includes catastrophic collisions and cratering events, and takes into account the stability and instability zones of the 3:2 mean motion resonance with Neptune. Our results suggest that if 1 Pluto-sized object is in this resonance, the flux of D = 2 km Plutinos on Pluto is ~4–24 percent of the flux of D = 2 km Kuiper Belt projectiles on Pluto. However, with 5 Pluto-sized objects in the resonance, the contribution of the Plutino population to the impactor flux on Pluto may be comparable to that of the Kuiper Belt. As for Charon, if 1 Pluto-sized object is in the 3:2 resonance, the flux of D = 2 km Plutinos is ~10–63 percent of the flux of D = 2 km impactors coming from the Kuiper Belt. However, with 5 Pluto-sized objects, the Plutino population may be a primary source of the impactor flux on Charon. We conclude that it is necessary to specify the Plutino size distribution and the number of Pluto-sized objects in the 3:2 Neptune resonance in order to determine if the Plutino population is a primary source of impactors on the Pluto-Charon system.

Keywords

Kuiper BeltSolar System: GeneralMethods: Numerical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S263: Icy Bodies of the Solar System , August 2009 , pp. 98 - 101
Copyright
Copyright © International Astronomical Union 2010

References

Benz, W. & Asphaug, E. 1999, Icarus, 142, 5CrossRefGoogle Scholar
Davis, D. R., Weidenschilling, S. J., Farinella, P., Paolicchi, P., & Binzel, R. P. 1989, in: Binzel, R. P., Gehrels, T. & Matthews, M. S. (eds.), Asteroids II, (Tucson: University of Arizona Press), p. 805Google Scholar
de Elía, G. C., Brunini, A., & Di Sisto, R. P. 2008, A&A, 490, 835Google Scholar
Dell'Oro, A., Marzari, F., Paolicchi, P., & Vanzani, V. 2001, A&A, 366, 1053Google Scholar
Durda, D. D. & Stern, S. A. 2000, Icarus, 145, 220CrossRefGoogle Scholar
Fernández, J. A., Gallardo, T., & Brunini, A. 2002, Icarus, 159, 358CrossRefGoogle Scholar
Kenyon, S. J., Bromley, B. C., O'Brien, D. P., & Davis, D. R. 2008, in: Barucci, M. A., Boehnhardt, H., Cruikshank, D. P., & Morbidelli, A. (eds.), The Solar System Beyond Neptune, (Tucson: University of Arizona Press), p. 293Google Scholar
Morbidelli, A. 1997, Icarus, 127, 1CrossRefGoogle Scholar
O'Brien, D. P. & Greenberg, R. 2005, Icarus, 178, 179CrossRefGoogle Scholar
Zahnle, K., Schenk, P., Levison, H., & Dones, L. 2003, Icarus, 163, 263CrossRefGoogle Scholar