Isolating the mechanisms for asteroid surface refreshing
F. E. DeMeo, M. Marsset, D. Polishook, B. J. Burt, R. P. Binzel, S., Hasegawa, M. Granvik, N. A. Moskovitz, A. Earle, S. J. Bus, C. A. Thomas, A., S. Rivkin, S. M. Slivan

TL;DR
This study investigates various mechanisms that could explain the presence of fresh surfaces on asteroids, analyzing spectral data of 477 asteroids to identify trends and suggest multiple processes are involved.
Contribution
It provides a comprehensive spectral analysis of a large asteroid sample, revealing new trends in surface freshness related to size, orbit, and inclination, and emphasizes the need for multiple resurfacing mechanisms.
Findings
Q/S ratio peaks near H=19 and at 5° inclination
Q/S ratio increases with decreasing perihelion distance
Multiple resurfacing mechanisms are likely involved
Abstract
Evidence is seen for young, fresh surfaces among Near-Earth and Main-Belt asteroids even though space-weathering timescales are shorter than the age of the surfaces. A number of mechanisms have been proposed to refresh asteroid surfaces on short timescales, such as planetary encounters, YORP spinup, thermal degradation, and collisions. Additionally, other factors such as grain size effects have been proposed to explain the existence of these "fresh-looking" spectra. To investigate the role each of these mechanisms may play, we collected a sample of visible and near-infrared spectra of 477 near-Earth and Mars Crosser asteroids with similar sizes and compositions - all with absolute magnitude H > 16 and within the S-complex and having olivine to pyroxene (ol/(ol+opx)) ratios > 0.65. We taxonomically classify these objects in the Q (fresh) and S (weathered) classes. We find four trends in…
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