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Surface Mapping of Earth-like Exoplanets using Single Point Light Curves
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A super-massive Neptune-sized planet
Luca Naponiello1,2,3,4, Luigi Mancini5,6,7, Alessandro Sozzetti6
1Department of Physics, University of Rome "Tor Vergata", Rome, Italy. lnaponiello@roma2.infn.it.
Nature
|August 30, 2023
Summary
The dense, Neptune-sized exoplanet TOI-1853 b, found in the hot-Neptune desert, challenges formation theories with its high mass and density. Its unusual composition may result from planet collisions or inward migration.
Area of Science:
- Exoplanetary Science
- Planetary Formation and Evolution
- Astrophysics
Background:
- Neptune-sized planets display diverse compositions and densities, influenced by formation location and atmospheric escape.
- These planets range from low-density, hydrogen-helium-rich worlds to denser planets with water or rocky interiors.
- The 'hot-Neptune desert' is a region near stars with a scarcity of Neptune-sized planets, offering clues to planetary system evolution.
Purpose of the Study:
- To report the discovery and characterization of the transiting exoplanet TOI-1853 b.
- To investigate the unusual properties of TOI-1853 b and its implications for planetary formation theories.
- To understand the formation and evolutionary pathways of planets within the hot-Neptune desert.
Main Methods:
- Observations of the transiting planet TOI-1853 b using transit photometry.
- Determination of the planet's radius (3.46 ± 0.08 Earth radii) and orbital period (1.24 days).
- Measurement of the planet's mass (73.2 ± 2.7 Earth masses) and calculation of its density (9.7 ± 0.8 g/cm³).
Main Results:
- TOI-1853 b is a Neptune-sized planet with a mass nearly double that of previously known planets in its size class.
- The planet's high density suggests a composition dominated by heavy elements, unlike typical Neptune-sized planets.
- Its location within the hot-Neptune desert and extreme density present a significant puzzle for current models.
Conclusions:
- TOI-1853 b's properties challenge conventional planetary formation and evolution theories.
- Its existence may be explained by multiple high-energy proto-planet collisions.
- Alternatively, it could represent the end state of a highly eccentric planet that migrated inward towards its host star.
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