14/07/2026
Located roughly 100 light-years away in the Draco constellation, the exoplanet TOI-1452 b represents a profound milestone in astrophysical exploration.
Discovered utilizing NASA's Transiting Exoplanet Survey Satellite (TESS) alongside ground-based instruments like the SPIRou spectropolarimeter, this "super-Earth" orbits an M-type red dwarf star within a binary star system.
Initial calculations indicate the planet is approximately 70% larger in diameter and nearly five times more massive than Earth.
The primary metric captivating the scientific community is the planet's unique volumetric mass distribution.
Computer modeling and mass-to-radius ratios suggest a bulk density far too low for a purely terrestrial composition of iron and silicate rock, yet far too dense to be a volatile gas giant.
Instead, internal structure simulations indicate that water could comprise up to 30% of the planet's total mass.
This compositional signature mirrors the high-volatile profiles of icy moons in our outer solar system, such as Ganymede and Enceladus, but on a massive, temperate planetary scale where the water remains entirely liquid.
Because the planet is situated within its host star's conservative habitable zone, astronomers theorize that its volatile inventory exists as a global, contiguous hydrosphere.
Unlike Earth's shallow oceans, which average a mere 3.7 kilometers in depth and account for less than 0.02% of our total planetary mass, the global ocean of TOI-1452 b is projected to extend down hundreds of kilometers before encountering a dense, high-pressure rocky core.
To definitively map this volatile architecture and rule out alternative models—such as a bare rocky world enveloped in a hydrogen-helium atmosphere—the system remains a priority target for transmission spectroscopy via the James Webb Space Telescope (JWST).
📷 Image is for representation purpose only
