A giant impact as the likely origin of different twins in the Kepler-107 exoplanet system

Measures of exoplanet bulk densities indicate that small exoplanets with radius less than 3 Earth radii (R⊕) range from low-density sub-Neptunes containing volatile elements¹ to higher-density rocky planets with Earth-like² or iron-rich³ (Mercury-like) compositions. Such astonishing diversity in observed small exoplanet compositions may be the product ofdifferent initial conditions of the planet-formation process or different evolutionary paths that altered the planetary properties after formation⁴. Planet evolution may be especially affected by either photoevaporative mass loss induced by high stellar X-ray and extreme ultraviolet (XUV) flux⁵ or giant impacts⁶. Although there is some evidence for the former^7,8, there are no unambiguous findings so far about the occurrence of giant impacts in an exoplanet system. Here, we characterize the two innermost planets ofthe compact and near-resonant system Kepler-107 (ref. ⁹). We show that they have nearly identical radii (about 1.5-1.6R⊕), but the outer planet Kepler-107 c is more than twice as dense (about 12.6 g cm-3) as the innermost Kepler-107 b (about 5.3 g cm-3). In consequence, Kepler-107 c must have a larger iron core fraction than Kepler-107 b. This imbalance cannot be explained by the stellar XUV irradiation, which would conversely make the more-irradiated and less-massive planet Kepler-107 b denser than Kepler-107 c. Instead, the dissimilar densities are consistent with a giant impact event on Kepler-107 c that would have stripped off part of its silicate mantle. This hypothesis is supported by theoretical predictions from collisional mantle stripping¹⁰, which match the mass and radius of Kepler-107 c.