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Official Journal of the Asia Oceania Geosciences Society (AOGS)

Geoscience Letters Cover Image
Fig. 5 | Geoscience Letters

Fig. 5

From: Asteroid spin-rate studies using large sky-field surveys

Fig. 5

This figure is reproduced from Chang et al. (2015, 2016)

Light-curve amplitude vs. spin rate (left) and spin-rate distribution (right) for the C- (upper) and the S-type (lower) asteroids. The gray and red filled circles are objects of the LCDB and the PTF-U2s, respectively. The number of asteroids used in the statistics is given in each plot. The spin-rate limits, \(P \sim 3.3 \sqrt{(1 + \Delta m)/\rho }\) (Pravec and Harris 2000), are represented by dashed, dot-dashed, and dotted lines for rubble-pile asteroids with bulk densities of \(\rho =\) 3, 2, and \(1\,\text{g}\,\text{cm}^{-3}\), respectively. The spin-rate distributions use only asteroids of \(3< D < 20\) km.

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