Hostname: page-component-76fb5796d-x4r87 Total loading time: 0 Render date: 2024-04-26T13:21:01.428Z Has data issue: false hasContentIssue false
  • English
  • Français

Dynamics of the Zodiacal Cloud

Published online by Cambridge University Press:  07 August 2017

S. F. Dermott ,
R. S. Gomes ,
D. D. Durda ,
B. Å. S. Gustafson ,
S. Jayaraman ,
Y. L. Xu  and
P. D. Nicholson
S. F. Dermott
Affiliation:
Department of Astronomy, University of Florida, Gainesville, FL 32611, USA
R. S. Gomes
Affiliation:
Observatório Nacional, Departamento de Astronomia, Rio de Janeiro, Brazil
D. D. Durda
Affiliation:
Department of Astronomy, University of Florida, Gainesville, FL 32611, USA
B. Å. S. Gustafson
Affiliation:
Department of Astronomy, University of Florida, Gainesville, FL 32611, USA
S. Jayaraman
Affiliation:
Department of Astronomy, University of Florida, Gainesville, FL 32611, USA
Y. L. Xu
Affiliation:
Department of Astronomy, University of Florida, Gainesville, FL 32611, USA
P. D. Nicholson
Affiliation:
Department of Astronomy, Cornell University, Ithaca, NY 14853, USA

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.

Advances in infrared astronomy and in computing power have recently opened up an interesting area of the solar system for dynamical exploration. The survey of the sky made by The Infrared Astronomical Satellite (IRAS) in 1983 revealed the complex structure of the zodiacal dust cloud. We now know the inclination and nodes of the plane of symmetry of the cloud with respect to the ecliptic and we have evidence that the cloud is not rotationally symmetric with respect to the Sun. Of even more interest is the discovery by IRAS of prominent dust bands that circle the Sun in planes near-parallel to the ecliptic. In 1984, we suggested (Dermott et al., Nature, 312, 505-509) that the solar system dust bands discovered by IRAS are produced by the gradual comminution of the asteroids in the major Hirayama asteroid families. The confirmation of this hypothesis has involved: (1) The development of a new secular perturbation theory that includes the effects of Poynting-Robertson light drag on the evolution of the dust particle orbits; (2) The production of a new high resolution Zodiacal History File by IPAC (the Infrared Processing and Analysis Center at Caltech); (3) The development of the SIMUL code: a three-dimensional numerical model that allows the calculation of the thermal flux produced by any particular distribution of dust particle orbits. SIMUL includes the effects of planetary perturbations and PR drag on the dust particle orbits and reproduces the exact viewing geometry of the IRAS telescope. We report that these tools allow us to account in detail for the observed structure of the dust bands. They also allow us to show that there is evidence in the IRAS data for the transport of asteroidal dust from the main belt to the Earth by Poynting-Robertson light drag.

Type
Part VI - Meteors. Zodiacal Cloud. Nebulae
Information
Symposium - International Astronomical Union , Volume 152: Chaos, Resonance and Collective Dynamical Phenomena in the Solar System , 1992 , pp. 333 - 347
Copyright
Copyright © Kluwer 1992 

References

Burns, J. A., Lamy, P. L. and Soter, S. (1979) Radiation Forces on Small Particles in the Solar System. Icarus , 40, 1–48.Google Scholar
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 Bands. IAU Colloquium #85 Properties and Interaction of Interplanetary Dust (eds. Giese, R. H. and Lamy, P.) D. Reidel Pub. Co., 395–409.Google Scholar
Dermott, S. F., Nicholson, (1986) Masses of the Satellites of Uranus. Nature , 319, 115–120.Google Scholar
Dermott, S. F., Nicholson, P. D. and Wolven, B. (1986) Preliminary Analysis of the IRAS Solar System Dust Band Data, In Asteroids, Comets and Meteors, II (eds. Lagerkvist, C-I. and Rickman, H.), Uppsala, 583–594.Google Scholar
Dermott, S. F., Nicholson, P. D., Kim, Y., Wolven, B. and Tedesco, E. (1988) The Impact of IRAS on Asteroidal Science. In Comets to Cosmology (ed. Lawrence, A.), Berlin, Springer Verlag, 3–18.CrossRefGoogle Scholar
Dermott, S. F. and Nicholson, P. D. (1989) IRAS Dustbands and the Origin of the Zodiacal Cloud. In Highlights of Astronomy 8, 259–26.Google Scholar
Dermott, S. F., Nicholson, P. D., Gomes, R. S. and Malhotra, R. (1990) Modelling the IRAS Solar System Dustbands. Adv. Space Res. 10, (1)165–(1)172.Google Scholar
Dermott, S. F., Durda, D. D., Gustafson, B. A. S., Jayaraman, S., Xu, Y. L., Gomes, R. S. and Nicholson, P. D. (1992) The Origin and Evolution of the Zodiacal Dust Cloud. In Asteroids, Comets and Meteors, IV (eds. Bowell, E. and Harris, A.), Flagstaff, in press.Google Scholar
Durda, D. D., Dermott, S. F. and Gustafson, B. A. S. (1992) Modeling of Asteroidal Dust Source Production Rates. In Asteroids, Comets and Meteors, IV , (eds. Bowell, E. and Harris, A.), Flagstaff, in press.Google Scholar
Flynn, G. J. (1992) Large Micrometeorites: Atmospheric Entry Survival Relation to Mainbelt Asteroids, and Implication for the Cometary Dust Flux. In Asteroids, Comets and Meteors, IV , (eds. Bowell, E. and Harris, A.), Flagstaff, in press.Google Scholar
Giese, R. H. and Kneißel, B. (1989) Three-Dimensional Models of the Zodiacal Dust Cloud. II. Compatibility of Proposed Infrared Models. Icarus, 81, 369–378.Google Scholar
Gomes, R. S. and Dermott, S. F. (1992). Icarus , (to be submitted).Google Scholar
Grün, E., et al., (1992) Interplanetary Dust Near 1 AU, In Asteroids, Comets and Meteors, IV , (eds, Bowell, E., and Harris, A.), Flagstaff, in press.Google Scholar
Gustafson, B. A. S. (1992) Thermal Emission from Asteroidal and Cometary Dust Models. Submitted to Icarus. Google Scholar
Gustafson, B. A. S., Dermott, S. F., Durda, D. D. and Grün, E. (1992) Collisional and Dynamical Evolution of Dust from the Asteroid Belt. In Asteroids, Comets and Meteors, IV , (eds. Bowell, E. and Harris, A.), Flagstaff, in press.Google Scholar
Levasseur, A-C. and Blamont, J. (1976) Evidence for Scattering Particles in Meteor Streams. In Interplanetary Dust and Zodiacal Light (eds. Elsasser, H. and Fechtig, H.), Springer-Verlag, Heidelberg, pp. 58–62.Google Scholar
Schramm, L. S., Brownlee, D., and Wheelock, M. M. (1989) Major Element Composition of Stratospheric Micrometeorites. Meteoritics , 99–112.CrossRefGoogle Scholar
Stephens, J. R. and Gustafson, B. A. S. (1991) Laboratory Reflectance Measurements of Analogues to “Dirty” Ice Surfaces on Atmosphereless Solar System Bodies. Icarus , 94, 209–217.Google Scholar
Wyatt, S. P. and Whipple, F. L. (1950) The Poynting-Robertson Effect on Meteor Orbits. Ap. J. , 111, 134–141.Google Scholar