Radar and optical observations of asteroid 1998 KY26

Science

Volumn 285, Issue 5427, 1999, Pages 557-559

  Ostro, Steven J ^a   Pravec, Petr ^b   Benner, Lance A M ^a   Hudson, R Scott ^c   Šarounová, Lenka ^b   Hicks, Michael D ^a   Rabinowitz, David L ^a   Scotti, James V ^d   Tholen, David J ^e   Wolf, Marek ^f   Jurgens, Raymond F ^a   Thomas, Michael L ^a   Giorgini, Jon D ^a   Chodas, Paul W ^a   Yeomans, Donald K ^a   Rose, Randy ^a   Frye, Robert ^a   Rosema, Keith D ^a   Winkler, Ron ^a   Slade, Martin A ^a  

^a CALIFORNIA INSTITUTE OF TECHNOLOGY   (United States)

^b ASTRONOMICAL INSTITUTE   (Czech Republic)

^c Washington State University   (United States)

^d UNIVERSITY OF ARIZONA   (United States)

^e UNIVERSITY OF HAWAII   (United States)

^f CHARLES UNIVERSITY   (Czech Republic)

Author keywords

[No Author keywords available]

Indexed keywords

ASTEROID; CARBONACEOUS CHONDRITE; ROTATION;

ARTICLE; ASTRONOMY; GRAVITY; PRIORITY JOURNAL; TOPOGRAPHY; VELOCITY;

ASTEROIDEA;

EID: 0033597881     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.285.5427.557     Document Type: Article

References (41)

1. D. L. Rabinowitz et al., Nature 363, 704 (1993).
2. D. L. Rabinowitz, E. Bowell, E. Shoemaker, K. Muinonen, in Hazards Due to Cornets and Asteroids, T. Gehrels, Ed. (Univ. of Arizona Press, Tucson, AZ, 1994), pp. 285-312.
3. Spacecraft flybys have imaged four asteroids, all with average overall dimensions between 14 and 58 km.
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8. -1.
9. We used B, V, R, and I color filters of the Johnson-Cousins system, with respective effective wavelengths of 440, 550, 650, and 800 nm [M. S. Bessell, Publ. Astron. Soc. Pac. 102, 1181 (1990)].
10. The physical range extent typically is about twice the visible range extent [R. S. Hudson and S. J. Ostro, Science 270, 84 (1995); A. K. Andrews, R. S. Hudson, D. Psaltis, Opt. Lett. 20, 2327 (1995)].
11. The physical range extent typically is about twice the visible range extent [R. S. Hudson and S. J. Ostro, Science 270, 84 (1995); A. K. Andrews, R. S. Hudson, D. Psaltis, Opt. Lett. 20, 2327 (1995)].
12. Asteroid 1998 KY26's period was determined unambiguously in independent data from three different stations (Ondfejov, Table Mountain, Spacewatch). Observational techniques and data reduction procedures were similar to those described by P. Pravec, L. Šarounová, and M. Wolf [Icarus 124, 471 (1996)] and by D. Rabinowitz [ibid. 134, 342 (1998)], and used an implementation of the Fourier method developed by A. W. Harris et al. [ibid. 77, 171 (1989)].
13. Asteroid 1998 KY26's period was determined unambiguously in independent data from three different stations (Ondfejov, Table Mountain, Spacewatch). Observational techniques and data reduction procedures were similar to those described by P. Pravec, L. Šarounová, and M. Wolf [Icarus 124, 471 (1996)] and by D. Rabinowitz [ibid. 134, 342 (1998)], and used an implementation of the Fourier method developed by A. W. Harris et al. [ibid. 77, 171 (1989)].
14. Asteroid 1998 KY26's period was determined unambiguously in independent data from three different stations (Ondfejov, Table Mountain, Spacewatch). Observational techniques and data reduction procedures were similar to those described by P. Pravec, L. Šarounová, and M. Wolf [Icarus 124, 471 (1996)] and by D. Rabinowitz [ibid. 134, 342 (1998)], and used an implementation of the Fourier method developed by A. W. Harris et al. [ibid. 77, 171 (1989)].
15. Rotation periods of near-Earth asteroids and similar-sized, main-belt asteroids average about 12 and 7 hours, respectively [D. F. Lupishko and M. DiMartino, Planet. Space Sci. 46, 47 (1998)].
16. The period of 1995 HM has been suggested to be 97.2 or 145.8 min [D. I. Steel, R. H. McNaught, G. J. Garradd, D. J. Asher, A. D. Taylor, Planet. Space Sci. 45, 1091 (1997)].
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18. -4 times values for rocks [J. Suppe, Principles of Structural Geology (Prentice-Hall, Englewood Cliffs, NJ, 1985), p. 155]. Thus, 1998 KY26 could be held together by very meager bonds.
19. -4 times values for rocks [J. Suppe, Principles of Structural Geology (Prentice-Hall, Englewood Cliffs, NJ, 1985), p. 155]. Thus, 1998 KY26 could be held together by very meager bonds.
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23. 7 years.
24. 7 years.
25. 7 years.
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38. 7 year dynamical lifetime of objects in Earth-crossing orbits.
39. 7 year dynamical lifetime of objects in Earth-crossing orbits.
40. E. Asphaug et al., Nature 393, 437 (1998).
41. Part of this research was conducted at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. Work at Washington State University was supported in part by NASA's Planetary Geology and Geophysics Program. Work at Ondřejov was supported by the Grant Agency of the Academy of Sciences of the Czech Republic.