The spin periods of M asteroids

Details The spin periods of M asteroids The spin periods of M asteroids

Jun 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981m%26p....24..437l&link_type=abstract

Moon and the Planets, vol. 24, June 1981, p. 437-440.

Astronomy and Astrophysics

Astronomy

17

Angular Velocity, Asteroids, Astronomical Photometry, Planetary Rotation, Ubv Spectra, Albedo, Light Curve, Planetology

Scientific paper

In an attempt to verify the suggestion by Harris and Burns (1979) that M-type asteroids in general have high spin rates, a program of photoelectric UBV observations of M and CMEU asteroids is currently under way. Recently, the rotation periods, light-curve amplitudes and UBV color indices have been determined for the asteroids 201 Penelope and 250 Bettina, both of which are situated in the (C,M,E) domain of the two-color diagram. The resulting periods are very short (cf., IAUC 3523 and 3527). In general, it is found 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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