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Combined analysis of Chang’e-3 in situ measurements and Chang’e-5 laboratory samples, with an updated chronology from Chang’e-5 data, reconstructed the relation between age and composition of young lunar mare basalts. Results indicate persistent volcanism 2 Gyr ago, indicative of the presence of a heat source at the time.
A planetary origin model that forms exoplanets from a narrow ring of silicate material at a stellocentric distance of 1 au is able to explain the physical properties of super-Earths and reproduce the ‘peas in a pod’ pattern of uniformity within planetary architecture.
An abrupt slow-down in a magnetar’s rotation rate (a ‘glitch’) may be related to the subsequent emission of three radio bursts (resembling fast radio bursts) and a month-long episode of pulsed radio emission.
The aqueous activity responsible for carbonate formation on Ryugu happened much earlier—less than 1.8 million years after CAI formation—than estimates (4–6 Myr) from carbonaceous chondrite meteorites. Ryugu’s parent body either was smaller than ∼20 km in diameter or was disrupted before reaching the high temperatures required.
MicrOmega characterized the population of carbonates detected in the bulk components and in individual grains of the Ryugu returned samples. Two main carbonate families are detected, which were likely formed via two distinct processes at different stages in the early Solar System.
Through mapping the gamma-ray flux in giant molecular clouds, it appears that low-energy cosmic rays hardly penetrate into dense, potentially star-forming, clumps. This finding implies a slower diffusion of cosmic rays in these clumps, possibly caused by higher levels of magnetic turbulence than anticipated.
From an end-to-end model that characterizes the host galaxy, environment and progenitors of the binary neutron star merger gravitational wave event GW170817, the preferred solution is 2 low-metallicity stars of >10 solar masses that were born during Cosmic Noon, interacted repeatedly and remained bound even through 2 supernovae.
Lunar high-concentration ferric ion (Fe3+/∑Fe > 40%) and ~63% of nanophase metallic iron (npFe0) are produced via charge disproportionation of ferrous iron from micrometeoroid impacts, as observed in the Chang’e-5 sample. This ongoing process would lead to a continuously increasing abundance of Fe3+ in the lunar regolith.