The spin periods of masteroids (original) (raw)

Abstract

In an attempt to verify the suggestion by Harris and Burns (1979) that M-type asteroids in general have high spin rates we are currently involved in a programme of photoelectric_UBV_ observations of M and CMEU asteroids. Recently we have thus determined rotation periods, light-curve amplitudes and_UBV_ colour indices for the asteroids 201 Penelope and 250 Bettina, both of which are situated in the (C,M,E) domain of the two-colour diagram. The resulting periods are very short (cf., IAUC 3523 and 3527). In general, we find that both the M and CMEU asteroid groups appear to be characterized by fast rotations, large amplitudes and an avoidance of membership in Hirayama families.

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Authors and Affiliations

1. Astronomiska Observatoriet, Uppsala, Sweden
   C. -I. Lagerkvist & H. Rickman

Authors

1. C. -I. Lagerkvist
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2. H. Rickman
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Based on observations partly obtained at the European Southern Observatory, La Silla, Chile.

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Lagerkvist, C.I., Rickman, H. The spin periods of masteroids.The Moon and the Planets 24, 437–440 (1981). https://doi.org/10.1007/BF00896909

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• Received: 24 November 1980
• Issue Date: June 1981
• DOI: https://doi.org/10.1007/BF00896909

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