The Dense Iron Core of Rocky Exoplanet GJ 367 b

The Dense Iron Core of Rocky Exoplanet GJ 367 b

A World of Unyielding Density

In the quiet reaches of the Vela constellation, approximately 31 light-years from our solar system, orbits a celestial body of extraordinary composition: GJ 367 b. Unlike the gas-dominated giants that populate much of the known exoplanetary catalog, this world is a testament to the extreme efficiency of planetary formation in close proximity to a red dwarf star. Classified as a sub-Earth, GJ 367 b possesses a radius roughly 72% that of Earth, yet it packs a density comparable to that of solid iron, suggesting an interior structure that is almost entirely metallic.

The Dense Iron Core of Rocky Exoplanet GJ 367 b - Section 1 overview

Orbital Dynamics and Thermal Extremes

The orbital mechanics of GJ 367 b are defined by an intense, rapid transit. Completing a full revolution around its host star in just 7.7 hours, the planet is subjected to constant, blistering radiation. Surface temperatures are estimated to reach levels exceeding 1,500 degrees Celsius, enough to maintain a state of permanent molten surface flux. Because the orbital period is so short, the planet is almost certainly tidally locked, with one hemisphere perpetually scorched by the host star's output, creating an extreme thermal gradient across its surface.


Geological Composition and Interior Structure

Geophysical modeling of GJ 367 b reveals a world that likely represents the stripped remains of a much larger planetary core. The absence of a substantial atmosphere is a direct consequence of the immense stellar wind pressure acting upon its surface, preventing the accumulation of volatile gases. The planet's high mass-to-radius ratio implies an internal composition dominated by an iron-nickel alloy, likely accounting for 80% to 90% of the total mass. The crust, while potentially cooled and solidified in certain stagnant regions, exists in a state of high-pressure geological equilibrium with the mantle.

The Dense Iron Core of Rocky Exoplanet GJ 367 b - Section 3 overview

Topographic Features and Surface Environment

Due to the extreme heat, the surface is not static. It is characterized by vast, flowing pools of molten basalt and exposed metallic crust. The topography is jagged and scarred by the lack of tectonic plate activity typical of more temperate worlds, yet it remains geologically active through massive volcanic outgassing and thermal expansion. Without the buffering effect of an atmosphere, the surface is exposed directly to the harsh electromagnetic spectrum of its parent star, resulting in a landscape of dark, scorched rock and shimmering, reflective metallic plains that glow faintly with thermal radiation.

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