S19A0064

The bulk density/interior structure of asteroid is important to understand asteroids themselves and the system they reside in. Instead of measuring asteroid bulk density using space mission, this information can be obtained through their common spin-rate limit. The main belt asteroids (MBAs) of D > 0.15 km show a 2-hr spin-rate limit, which was explained using the rubble-pile structure (i.e., gravitationally bounded aggregations) and an upper limit of bulk density of ∼ 3 g cm−3 (Harris 1996). Although a 5-hr spin-rate limit was pointed out (Szabo et al. 2017, Ryan et al. 2017) for Jovian Trojans (JTs) of D > 10 km, a faster averaged spin-rate for smaller objects, as seen in MBAs of D < 10 km, is possible to happen in JTs of D < 10 km as well. Therefore, we must obtain the rotation-period distribution of small JTs (D < 10 km) to confirm the 5-hr limit to probe the JT’s bulk density. Once this limit is confirmed, it is interesting to know any super-fast rotator (SFR, rotation period over the limit) in JTs? Moreover, the spin-rate distribution, binary fraction, and shape distribution of JTs will also be available to conduct a comparative study with other asteroid groups. The wide FOV and deep magnitude observation of HSC-Subaru is the only choice to conduct this survey.


This document was translated from LATEX by HEVEA.