A 100,000-year periodicity in the accretion rate of interplanetary dust

Science

Volumn 280, Issue 5365, 1998, Pages 874-876

  Kortenkamp, Stephen J ^a   Dermott, Stanley F ^b  

^a GEOPHYSICAL LABORATORY   (United States)

^b 211 Space Sciences Building ^*  (United States)

Author keywords

[No Author keywords available]

Indexed keywords

HELIUM;

ARTICLE; ASTRONOMY; DUST; PERIODICITY; PRIORITY JOURNAL; SEDIMENT;

EID: 0032496303     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.280.5365.874     Document Type: Article

References (45)

1. E. Grün, H. A. Zook, H. Fechtig, R. H. Giese, Astron. Astrophys. 286, 915 (1985); S. G. Love and D. E. Brownlee, Science 262, 550 (1993).
2. E. Grün, H. A. Zook, H. Fechtig, R. H. Giese, Astron. Astrophys. 286, 915 (1985); S. G. Love and D. E. Brownlee, Science 262, 550 (1993).
3. G. W. Wetherill, Geochim. Cosmochim. Acta. 40, 1297 (1976).
4. J. P. Bradley, S. A. Sandford, R. M. Walker, in Meteorites and the Early Solar System, J. F. Kerridge and M. Matthews, Eds. (Univ. of Arizona, Tucson, AZ, 1988), pp. 861-895.
5. S. P. Wyatt and F. L. Whipple, Astrophys. J. 111, 134 (1950).
6. Dermott et al. (24) state that de/dt applies to the proper e values. The forced e values also decay, but these must be calculated numerically [S. F. Dermott et al., in Chaos, Resonance and Collective Dynamical Phenomena in the Solar System, S. Ferraz-Mello, Ed. (Kluwer, Dordrecht, Netherlands, 1992), pp. 333-347].
7. B. Å. S. Gustafson, Annu. Rev. Earth Planet. Sci. 22, 553 (1994).
8. F. L. Whipple, Smithsonian Astrophys. Obs. Spec. Rep. 239, 1 (1967).
9. F. J. Low et al., Astrophys. J. Lett. 278, L19 (1984). The ecliptic is the plane of Earth's orbit.
10. S. F. Dermott, P. D. Nicholson, J. A. Burns, J. R. Houck, Nature 312, 505 (1984).
11. Dermott et al. (17) estimated that emission from dust from the Eos, Themis, and Koronis asteroid families may constitute 10% of the peak flux detected in the IRAS 25-μm wave band, whereas Grogan et al. (29) refined this estimate to as much as 25%. Reach et al. (33) found that 12% of the peak flux detected in the 25-μm wave band of the Cosmic Background Explorer (COBE) satellite may be due to dust from the Eos family alone.
12. S. J. Kortenkamp and S. F. Dermott, in preparation; S. J. Kortenkamp, thesis, University of Florida, Gainesville (1996).
13. G. J. Flynn, Proc. Lunar Planet. Sci. Conf. 20, 363 (1990); E. J. Öpik, Proc. R. Irish Acad. Sect. A 54, 165 (1951).
14. G. J. Flynn, Proc. Lunar Planet. Sci. Conf. 20, 363 (1990); E. J. Öpik, Proc. R. Irish Acad. Sect. A 54, 165 (1951).
15. D. J. Kessler, Icarus 48, 39 (1981).
16. Dermott et al. (17) estimated that emission from dust from all asteroidal sources may constitute 30% or more of the peak zodiacal emission, whereas Grogan et al. (29) put the estimate at 75%. Jayaraman and Dermott (34) estimated that anywhere from 10 to 100% of all IDPs near 1 AU could be asteroidal. Reach et al. (33) found evidence in the COBE data for dust bands associated with at least five and possibly seven asteroid families. They stated that "if nonfamily asteroids produce dust at a rate that is similar to the dusty asteroid families, asteroidal dust could account for the entire zodiacal" cloud (33, p. 481).
17. R. A. Muller and G. J. MacDonald, Science 277, 215 (1997).
18. The invariable plane of the solar system is perpendicular to the total orbital angular momentum vector of the planets.
19. S. F. Dermott, S. Jayaraman, Y. L. Xu, K. Grogan, B. Å. S. Gustafson, in Unveiling the Cosmic Infrared Background, E. Dwek, Ed. (Woodbury, New York, 1996), pp. 25-36.
20. T. R. Quinn, S. Tremaine, M. Duncan, Astron. J. 101, 2287 (1991).
21. E. Everhart, in Dynamics of Comets: Their Origin and Evolution, A. Carusi and G. B. Valsecchi, Eds. (Reidel, Dordrecht, Netherlands, 1985), pp. 185-202.
22. -3, these β values correspond to diameters of about 10 and 20 μm. However, our modeling is only dependent on β, so the results apply equally well to any combination of size, density, and composition that gives β values of 0.0469 and 0.0235. The code runs optimally when the number of secondary bodies is a power of 2, so we populated each wave with 249 dust particles in addition to the seven planets.
23. K. A. Farley and D. B. Patterson, Nature 378, 600 (1995).
24. K. A. Farley, S. G. Love, D. B. Patterson, Geochim. Cosmochim. Acta. 61, 2309 (1997).
25. F. Marcantonio et al., Nature 383, 705 (1996).
26. S. F. Dermott, S. Jayaraman, Y. L. Xu, B. Å. S. Gustafson, J. C. Liou, ibid. 369, 719 (1994).
27. Numerical simulations and IRAS observations (24) have shown that Earth shepherds a circumsolar resonant ring of asteroidal dust and that the planet is embedded in this ring with a cloud of dust permanently in its wake. Confirmation of this ring was found in the COBE observations [W. T. Reach et al., Nature 374, 521 (1995)].
28. K. A. Farley, Nature 376, 153 (1995).
29. B. Schmitz, B. Peucker-Ehrenbrink, M. Lindström, M. Tassinari, Science 278, 88 (1997).
30. -3) was estimated from tracking data and images obtained during the flyby of the Near Earth Asteroid Rendezvous spacecraft [D. K. Yeomans et al., Science 278, 2106 (1997); J. Veverka et al., ibid., p. 2109].
31. -3) was estimated from tracking data and images obtained during the flyby of the Near Earth Asteroid Rendezvous spacecraft [D. K. Yeomans et al., Science 278, 2106 (1997); J. Veverka et al., ibid., p. 2109].
32. -3) was estimated from tracking data and images obtained during the flyby of the Near Earth Asteroid Rendezvous spacecraft [D. K. Yeomans et al., Science 278, 2106 (1997); J. Veverka et al., ibid., p. 2109].
33. -3) was estimated from tracking data and images obtained during the flyby of the Near Earth Asteroid Rendezvous spacecraft [D. K. Yeomans et al., Science 278, 2106 (1997); J. Veverka et al., ibid., p. 2109].
34. -3) was estimated from tracking data and images obtained during the flyby of the Near Earth Asteroid Rendezvous spacecraft [D. K. Yeomans et al., Science 278, 2106 (1997); J. Veverka et al., ibid., p. 2109].
35. -3) was estimated from tracking data and images obtained during the flyby of the Near Earth Asteroid Rendezvous spacecraft [D. K. Yeomans et al., Science 278, 2106 (1997); J. Veverka et al., ibid., p. 2109].
36. K. Grogan, S. F. Dermott, S. Jayaraman, Y. L. Xu, Planet. Space Sci. 45, 1657 (1998).
37. M. R. Rampino, S. Self, R. B. Stothers, Annu. Rev. Earth Planet. Sci. 16, 73 (1988).
38. J. Wisdom, Icarus 56, 51 (1983); Nature 315, 731 (1985).
39. J. Wisdom, Icarus 56, 51 (1983); Nature 315, 731 (1985).
40. Gradual mass extinctions may have begun in the Late Cretaceous at least 100,000 years before the Cretaceous-Tertiary boundary impact 65 million years ago, and they extend 300,000 years into the Tertiary [G. Keller, E. Barrera, B. Schmitz, E. Mattson, Geol. Soc. Am. Bull. 105, 979 (1993)].
41. 3He-bearing interplanetary dust particles was increased for several million years across the Eocene-Oligocene transition.
42. W. T. Reach, B. A. Franz, J. L. Weiland, Icarus 127, 461 (1997).
43. S. Jayaraman and S. F. Dermott, in Physics, Chemistry and Dynamics of Interplanetary Dust, B. Å. S. Gustafson and M. S. Hanner, Eds. (Astronomical Society of the Pacific, San Francisco, CA, 1996), pp. 155-158.
44. B. T. Draine and H. M. Lee, Astrophys. J. 285, 89 (1984). "Astronomical silicate" is a hypothetical material defined by a table of optical properties (absorption and emission coefficients) that match the silicate features observed in interstellar dust.
45. We thank G. Wetherill, A. Boss, and two anonymous reviewers for their comments.