The Scorched Basaltic Crust of Rocky Super-Earth GJ 1132 b

Orbiting a dim red dwarf star just 39 light-years from our solar system, GJ 1132 b stands as a premier example of a high-density, rocky super-Earth. With a radius approximately 1.2 times that of our home world and a mass significantly greater, this body presents a geological profile defined by intense stellar proximity and extreme thermal exposure. Its tight, 1.6-day orbital period ensures that the surface remains perpetually baked by the radiation of its parent star, stripping away lighter volatile elements and leaving behind a composition likely dominated by silicate rock and iron.

The Scorched Basaltic Crust of Rocky Super-Earth GJ 1132 b - Section 1 overview

Geologically, GJ 1132 b is classified as a terrestrial world, though its environment is far removed from the temperate conditions of the inner solar system. The extreme heat flux from the M-dwarf host has likely led to a stagnant lid tectonic regime. Unlike worlds with active plate boundaries, the crust of GJ 1132 b appears to be a single, monolithic shell of volcanic rock. This lack of subduction processes contributes to the persistence of high-pressure geological features, where the internal heat is primarily managed through conductive cooling and limited, highly localized volcanic venting rather than the convective recycling seen on larger, more dynamic bodies. Much like the nitrogen-rich surfaces of cooler distant bodies, the crust here is shaped by persistent, intense thermal stress.

The atmospheric profile of this super-Earth is a subject of significant observational interest. Due to its proximity to the star, the primordial atmosphere was likely subjected to significant hydrodynamic escape. What remains is a secondary atmosphere, potentially rich in heavier species such as hydrogen, carbon dioxide, or even trace water vapor liberated from the interior mantle. High-resolution spectroscopy suggests that the atmosphere is thin and heavily irradiated, lacking the shielding of a robust, global magnetic field. This interaction between stellar wind and the rocky crust results in a dynamic, high-energy environment where the surface is constantly scoured by plasma interactions.

The interior structure of GJ 1132 b is characterized by a high-density core, likely composed of an iron-nickel alloy, overlain by a deep, silicate-rich mantle. The pressure at the core-mantle boundary is sufficient to ensure a distinct phase transition in the mineralogy, with silicates potentially adopting high-pressure crystalline structures that are rarely observed under surface conditions. The heat generated during the formation of the body, coupled with radioactive decay in the core, drives the thermal evolution of this world, making it a laboratory for studying the long-term cooling of high-mass terrestrial objects.

Ultimately, this world represents the harsh end-member of planetary formation. It exists as a perfectly bare, unobstructed sphere floating in completely empty space with nothing circling its equator. The physical surface remains a testament to the destructive power of stellar irradiation, providing a stark look at the final stages of planetary evolution where only the most refractory materials can remain stable. Its study allows astronomers to calibrate models for interior thermal profiles and atmospheric loss on super-Earths, offering a clearer view of the diversity of rocky worlds populating our local galaxy.

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