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Signatures of phyllosilicate-like hydrated minerals are widespread on Bennu’s surface, indicating significant aqueous alteration. The lack of spatial variations in the spectra down to the scale of ~100 m indicates both a relatively uniform particle size distribution and a lack of compositional segregation, possibly due to surficial redistribution processes.
Bennu’s surface has experienced continuous changes, mostly induced by its accelerating spin rate, which could have resulted in a collapse of its interior in the past. This scenario is also supported by the heterogeneity of Bennu’s internal mass distribution.
The iodine–xenon record in meteorites can be used to probe late-time processes within the Solar System, during the dissipation of its debris disk. Most primitive meteorites were processed and heated by impacts during this ~50 Myr period, rather than by the decay of 26Al.
LOFAR radio observations, complemented by ultraviolet and visible light images, of the powerful class-X8.2 solar flare of 10 September 2017 pinpoint the location of multiple shock signatures of electron beams (herringbones) along the expanding coronal mass ejection.
