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Iras Dust Bands and the Origin of the Zodiacal Cloud

Published online by Cambridge University Press:  14 August 2015

S. F. Dermott  and
P. D. Nicholson
S. F. Dermott
Affiliation:
Center for Radiophysics and Space Research, Cornell University, Ithaca, NY 14853, USA
P. D. Nicholson
Affiliation:
Center for Radiophysics and Space Research, Cornell University, Ithaca, NY 14853, USA

Abstract

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Previous discussions of the origin of the zodiacal cloud have attempted to distinguish between an asteroidal and a cometary source on the basis of collisional dynamics, that is, by calculating the rates of production and destruction of particles from the two possible sources. The uncertainties in these calculations are too large to permit a useful conclusion. The recognition that the solar system dust bands discovered by IRAS are probably produced by the gradual comminution of the asteroids in the major Hirayama asteroid families may allow us to estimate, with comparative confidence, the contribution to the zodiacal cloud of the asteroid belt as whole.

Type
Joint Discussions
Information
Highlights of Astronomy , Volume 8: Highlights of Astronomy. As presented at the XXth General Assembly of the IAU, 1988 , 1989 , pp. 259 - 266
Copyright
Copyright © Kluwer 1989

References

Dermott, S. F., Nicholson, P. D., Burns, J. A., and Houck, J. R. (1984) “Origin of the solar system dust bands discovered by IRAS”, Nature, 312, 505–509.Google Scholar
Dermott, S. F., Nicholson, P. D., Burns, J. A., and Houck, J. R. (1985) ‘An analysis of IRAS’ solar system dust band data’, In “Properties and interaction of interplanetary dust”, eds. Giese, R. H. and Lamy, P., Riedel, Dordrecht, 395–409.CrossRefGoogle Scholar
Dermott, S. F., Nicholson, P. D., and Wolven, B. (1986) ‘Preliminary analysis of the IRAS solar system dust data’, In “Asteroids, Comets and Meteors, II, eds. Lagerkvist, C-I. and Rickman, H., Uppsala, pp. 583–594.Google Scholar
Dermott, S. F., Nicholson, P. D., Kim, Y., and Wolven, B. (1988a) ‘The impact of IRAS on asteroidal science’, In “Comets to Cosmology”, ed. Lawrence, A., Springer-Verlag, Berlin, pp. 3–18.Google Scholar
Dermott, S. F., Nicholson, P. D., Gomes, R., and Malhotra, R. (1988b). “Modelling the IRAS solar system dust bands”, Adv. Space Res. (in press).Google Scholar
Dermott, S. F., and Gomes, R. (1988c). “Orbital decay of asteroidal dust particles due to Poynting-Robertson light drag and the origin of interplanetary dust particles” Icarus (submitted).Google Scholar
Dohnanyi, J. S. (1969) “Collisional model of asteroids and their debris”, J. Geophys. Res., 74, 2531–2554.Google Scholar
Low, F. J. et al. (1984) “Infrared cirrus: new components of the extended infrared emission”, Astroph. J. (Letters) 278, L19.Google Scholar
Neugebauer, G. et al. (1984) “Early results from the infrared astronomical satellite”, Science, 224, 14–21.Google Scholar
Schramm., L. S., Brownlee, D., and Wheelock, M. M. (1988) “Major element composition of stratospheric micrometeorites”, Meteoritics (in press).CrossRefGoogle Scholar
Sykes, M. V. and Greenberg, R. J. (1986) “The formation and origin of the IRAS zodiacal dust bands as a consequence of single collisions between asteroids”, Icarus, 65, 51–69.Google Scholar
Sykes, M. V. “IRAS observations of extended zodiacal structures”, Astrophys. J. (Letters), 334, (in press).Google Scholar