We detect a transiting rocky planet with an orbital period of 1.467 days around the nearby red dwarf star Gliese 486. The planet Gliese 486 b is 2.81 Earth masses and 1.31 Earth radii, a composition similar to that of Venus or Earth, as determined from exquisite radial velocity data and photometric light curves. The host star is at a distance of 26 light-years, very bright, and observable from both hemispheres of Earth. The stellar and planet properties indicate that despite the hot surface temperatures it is possible that the planet conserved part of its original atmosphere, making it an

Modelling dust formation in single stars evolving through the carbon-star stage of the asymptotic giant branch (AGB) (i.e., the late evolutionary stages of Sun-like stars) reproduces reasonably well the mid-infrared colours and magnitudes of most of the C-rich sources in low-metallicity galaxies with known distances like the Large Magellanic Cloud (LMC). The only exception to this is a small subset of extremely red objects (EROs). An analysis of the spectral energy distributions of EROs suggests the presence of large quantities of dust, which demand gas densities in the outflow significantly

Hayabusa2’s optical navigation camera (ONC) found many anomalously bright boulders on the dark surface of the carbonaceous (or C-type) asteroid Ryugu. Observations with ONC and the near-infrared spectrometer (NIRS3) indicates that at least six of those bright boulders exhibit reflectance spectra consistent with exogenous origin; their spectra are similar to rocky (or S-type) asteroids. This means that the bright boulders resulted from collisional mixing between Ryugu’s parent body and S-type asteroid(s). On Bennu, the asteroid explored by NASA’s OSIRIS-REx, bright boulders with spectra