The Spin-Barrier Ratio for S and C-Type Main Asteroids Belt

Abstract

Asteroids of size larger than 0.15 km generally do not have periods P smaller than about 2.2 hours, a limit known as cohesionless spin-barrier. This barrier can be explained by means of the cohesionless rubble-pile structure model. In this paper we will explore the possibility for the observed spin-barrier value to be different for C and S-type Main Asteroids Belt (MBAs). On the basis of the actual bulk density values, the expected ratio between the maximum rotation periods is $P_C/P_S\approx 1.4\pm 0.3$. Using the data available in the asteroid LightCurve Data Base (LCDB) we have found that, as regards the mean spin-barrier values and for asteroids in the 4-20 km range, there is a little difference between the two asteroids population with a ratio $P_C/P_S\approx 1.20\pm 0.04$. Uncertainties are still high, mainly because of the small number of MBAs with known taxonomic class in the considered range. In the 4-10 km range, instead, the ratio between the spin-barriers seems closer to 1 because $P_C/P_S\approx 1.11\pm 0.05$. This behavior could be a direct consequence of a different cohesion strength for C and S-type asteroids of which the ratio can be estimated.

10 pages, 6 figures

References in corpus (2)

• A possible YORP effect on C and S Main Belt Asteroids
• Statistical analysis of C and S Main Belt Asteroids

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