Hostname: page-component-78c5997874-ndw9j Total loading time: 0 Render date: 2024-11-03T00:27:44.070Z Has data issue: false hasContentIssue false
  • English
  • Français

Collisional Origin of Asteroid Families: Effects of the Target's Gravity

Published online by Cambridge University Press:  12 April 2016

Vincenzo Zappalà ,
Paolo Farinella  and
Paolo Paolicchi
Vincenzo Zappalà
Affiliation:
Osservatorio Astronomico di Torino, Pino Torinese, Italy
Paolo Farinella
Affiliation:
Scuola Normale Superiore and Dipartimento di Matematica dell'Università, Pisa, Italy
Paolo Paolicchi
Affiliation:
Osservatorio Astronomico di Brera, Merate, Italy

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The outcomes of asteroidal catastrophic collisions are strongly affected by the target asteroid's gravity, since only the fragments escaping with initial velocities higher than the target's escape velocity are not reaccumulated into “rubble pile” remnants. This idea can be compared with the observational evidence on the properties of family asteroids in several ways : (1) the shape and spin period of the “reaccumulated” family asteroids will roughly fit the relationships valid for self-gravitating fluid bodies; (2) the relative velocities of the few escaping fragments arising from a breakup event marginally overcoming self-gravity will often have an anisotropic distribution, affecting the final distribution of orbital elements; (3) the amount of mass which in a given family escaped to “infinity” will be correlated with the target's size, since only for objects larger than ~ 100 km self-gravity plays an important role. These predictions are discussed and compared with the available data.

Type
Part III - Asteroids
Information
International Astronomical Union Colloquium , Volume 74: Dynamical Trapping and Evolution in the Solar System , 1983 , pp. 177 - 188
Copyright
Copyright © Reidel 1983

References

Bowell, E., Gehrels, T., and Zellner, B.: 1979, in Asteroids (Gehrels, T. Ed.), 1108–1129, University of Arizona Press, Tucson.Google Scholar
Carusi, A., and Valsecchi, G.B.: 1982, Astron. Astrophys., in press.Google Scholar
Chandrasekhar, S.: 1969, Ellipsoidal Figures of Equillibrium, Yale University Press, New Haven and London.Google Scholar
Davis, D.R., Chapman, CR., Greenberg, R., Weidenschilling, S.J., and Harris, A.W.: 1979, in Asteroids (Gehrels, T. Ed.), pp. 528–557, University of Arizona Press, Tucson.Google Scholar
Farinella, P., Paolicchi, P., Tedesco, E.F., and Zappalà, V.: 1981, Icarus 46, pp. 114–123.CrossRefGoogle Scholar
Farinella, P., Paolicchi, P., and Zappalà, V.: 1982, Icarus, in press.Google Scholar
Farinella, P., Milani, A., Nobili, A.M., Paolicchi, P., and Zappalà, V.: 1983, Icarus, in press.Google Scholar
Fujiwara, A., Kamimoto, G., and Tsukamoto, A.: 1977, Icarus 31, pp. 277–288.CrossRefGoogle Scholar
Fujiwara, A., and Tsukamoto, A.: 1980, Icarus 44, pp. 142–153.CrossRefGoogle Scholar
Fujiwara, A.: 1982, submitted to Icarus.Google Scholar
Gradie, J.C., Chapman, C.R., and Williams, J.G.: 1979, in Asteroids (Gehrels, T. Ed.), pp. 359–390, University of Arizona Press, Tucson.Google Scholar
Ip, W.-H.:1979, Icarus 40, pp. 418–422.CrossRefGoogle Scholar
Kresák, L.:1977, Bull. Astron. Inst. Czech. 28, pp. 65–82.Google Scholar
Paolicchi, P., Farinella, P., and Zappalà, V.: 1982, in Sun and planetary system (Fricke, W. and Teleki, G. Eds.), pp. 295–298, D. Reidel, Dordrecht, Holland.CrossRefGoogle Scholar
Tedesco, E.F.: 1979, Icarus 40, pp. 375–382.CrossRefGoogle Scholar
Weidenschilling, S.J.: 1981, Icarus 46, pp. 124–126.CrossRefGoogle Scholar
Wiesel, W.: 1978, Icarus 34, pp. 99–116.CrossRefGoogle Scholar
Williams, J.G.: 1979, in Asteroids (Gehrels, T. Ed.), pp 1040–1063, University of Arizona Press, Tucson.Google Scholar