Composition and size of Apollo asteroid 1984 KB

Jeffrey F. Bell; Robert Hamilton Brown; B. Ray Hawke

doi:10.1016/0019-1035(88)90057-7

Composition and size of Apollo asteroid 1984 KB

Jeffrey F. Bell, Robert Hamilton Brown, B. Ray Hawke

Research output: Contribution to journal › Article › peer-review

6 Scopus citations

Abstract

Reflection spectra and thermal-emission radiometry were obtained for the Earth-crossing asteroid 1984 KB. The spectrum exhibits the spectral signatures of olivine, pyroxene, and NiFe metal; it is typical of Class S objects and suggests a surface material similar to the rare lodranite meteorites. A standard asteroid thermal model implies a radius of ∼0.7 km and an albedo of ∼0.16 (similar to Class S objects). An analysis of the same thermal data with a bare-rock thermal model gives an albedo inconsistent with the IR spectrum, suggesting that this object has a significant regolith despite its small size.

Original language	English (US)
Pages (from-to)	482-486
Number of pages	5
Journal	Icarus
Volume	73
Issue number	3
DOIs	https://doi.org/10.1016/0019-1035(88)90057-7
State	Published - Mar 1988
Externally published	Yes

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1016/0019-1035(88)90057-7

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title = "Composition and size of Apollo asteroid 1984 KB",

abstract = "Reflection spectra and thermal-emission radiometry were obtained for the Earth-crossing asteroid 1984 KB. The spectrum exhibits the spectral signatures of olivine, pyroxene, and NiFe metal; it is typical of Class S objects and suggests a surface material similar to the rare lodranite meteorites. A standard asteroid thermal model implies a radius of ∼0.7 km and an albedo of ∼0.16 (similar to Class S objects). An analysis of the same thermal data with a bare-rock thermal model gives an albedo inconsistent with the IR spectrum, suggesting that this object has a significant regolith despite its small size.",

author = "Bell, {Jeffrey F.} and Brown, {Robert Hamilton} and Hawke, {B. Ray}",

note = "Funding Information: The spectral observations were made possible by the Mauna Kea support staff, who communicated the preliminary ephemeris, and Bill Golisch, who con-vetted it to an accurate hourly ephemeris with his own computer. This work was supported by NASA Grant NAGW 802 to the University of Hawaii and also represents one phase of research carried out at the Jet Propulsion Laboratory under contract to the National Aeronautics and Space Administration.",

year = "1988",

month = mar,

doi = "10.1016/0019-1035(88)90057-7",

language = "English (US)",

volume = "73",

pages = "482--486",

journal = "Icarus",

issn = "0019-1035",

publisher = "Academic Press Inc.",

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TY - JOUR

T1 - Composition and size of Apollo asteroid 1984 KB

AU - Bell, Jeffrey F.

AU - Brown, Robert Hamilton

AU - Hawke, B. Ray

N1 - Funding Information: The spectral observations were made possible by the Mauna Kea support staff, who communicated the preliminary ephemeris, and Bill Golisch, who con-vetted it to an accurate hourly ephemeris with his own computer. This work was supported by NASA Grant NAGW 802 to the University of Hawaii and also represents one phase of research carried out at the Jet Propulsion Laboratory under contract to the National Aeronautics and Space Administration.

PY - 1988/3

Y1 - 1988/3

N2 - Reflection spectra and thermal-emission radiometry were obtained for the Earth-crossing asteroid 1984 KB. The spectrum exhibits the spectral signatures of olivine, pyroxene, and NiFe metal; it is typical of Class S objects and suggests a surface material similar to the rare lodranite meteorites. A standard asteroid thermal model implies a radius of ∼0.7 km and an albedo of ∼0.16 (similar to Class S objects). An analysis of the same thermal data with a bare-rock thermal model gives an albedo inconsistent with the IR spectrum, suggesting that this object has a significant regolith despite its small size.

AB - Reflection spectra and thermal-emission radiometry were obtained for the Earth-crossing asteroid 1984 KB. The spectrum exhibits the spectral signatures of olivine, pyroxene, and NiFe metal; it is typical of Class S objects and suggests a surface material similar to the rare lodranite meteorites. A standard asteroid thermal model implies a radius of ∼0.7 km and an albedo of ∼0.16 (similar to Class S objects). An analysis of the same thermal data with a bare-rock thermal model gives an albedo inconsistent with the IR spectrum, suggesting that this object has a significant regolith despite its small size.

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VL - 73

SP - 482

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JO - Icarus

JF - Icarus

IS - 3

ER -

Composition and size of Apollo asteroid 1984 KB

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