Now posted, the Meteoritics & Planetary Science October (vol. 60 #10) issue:
Rezes, D. Gyollai, I. Biri, S. et al. Comparison of three proton irradiated meteorite samples to better understand the solar wind-based space weathering Pgs 2297 maps.70038
Suttle, M. D. Findlay, R. Franchi, I. A. et al. Isotopic analysis of tochilinite (carbonate and magnetite) in Winchcombe: Temperature constraints on early-stage aqueous alteration in the… Pgs 2359 maps.70043
My usual caution: there are actually more papers in there that are relevant- some of them happen to be more relevant than others, your opinion may (likely should) differ from mine.
For years now, researchers have simulated space weathering on asteroids, by bombarding meteorites thought to be derived from asteroid parents. In the case of the solar wind, plus a lesser contribution from cosmic rays, bodies in space are hit by a faint but steady shower of hydrogen ions (basically, protons). We can simulate this in a lab: proton beams, with the appropriate energies, will alter minerals. Since many minerals (including asteroids) are silicates (based on the silicate tetrahedron, [SiO4]–), the combination of hydrogen with oxygen results in water. Yes, water in space.
Some of the more water-rich meteorites are the carbonaceous chondrite meteorites. Of the CC meteorites, the most common group within them are the CM chondrite meteorites. A recent fall of a CM meteorite was the Winchcombe, UK specimen, of which many fragments were recovered within hours, with little contact from our Biosphere. Authors Suttle et al. then post more results from analyzing that meteorite. Of the CM stones, the most common mineral is “TCI”- tochilinite-cronstedtite intergrowth. These are phyllosilicates (“clays”) in which there are both molecular-scale sheets of tochilinite, between molecular-scale sheets of- yeas- cronstedtite. These molecular sheets not only retain water, but signs of their formation. And thus, signs of the history of CM meteorites.