S18A0076abst
S18A0076
The bulk density/interior structure of asteroids is important to understand asteroids themselves and the system they reside in as well. Instead of direct mass measurement via space mission, a straightforward statistics on asteroid rotation periods (RPs) can reveal this information. The main belt asteroids (MBAs) of D > 150 meter show a 2-hr spin-barrier, which was explained by the rubble-pile structure (i.e., gravitationally bounded aggregations) with an upper limit of bulk density of 2.7 g cmβ3 (Harris 1996). Although a possible 5-hr spin-barrier was pointed out (Szabo et al. 2017, Rayn et al. 2017) using RPs of Jovian Trojans (JTs) of D > 10 km using K2 mission, a spin-rate transition could also happen to JTs of D βΌ 10 km as seen in MBAs. Therefore, a survey on the rotation periods of small JTs (i.e., D < 10 km) helps to confirm this 5-hr spin barrier and help to probe JTs bulk density. It is also interesting know any super-fast rotator (SFR, a RP breaks the spin barrier) in JTs and how they are compared to MBA SFRs? In addition, an un-biased spin-rate distribution, the binary fraction, and the shape distribution of JTs can also be obtained to conduct a comparative study with other asteroid groups. The wide FOV and large aperture of HSC/Subaru is the only choice to conduct this survey.
This document was translated from LATEX by HEVEA.