TOI-1472 c
Astrophysical Synthesis & Habitability Characterization
TOI-1472 c is a confirmed sub-neptune exoplanet orbiting the star TOI-1472, located approximately 397.4 light-years (121.84 parsecs) from the Solar System. First announced in 2025 by Multiple Observatories using the Radial Velocity detection technique (measuring periodic Doppler reflex motion in the host star's spectrum), this world measures 3.334 Earth radii (0.3 Jupiter radii) and has a measured mass of 21.13 Earth masses. Combining its mass and radius yields a mean bulk density of 3.14 g/cm³ (an intermediate density indicative of a deep water-ice mantle or dense volatile envelope), a surface gravity of 1.9 g⊕ (18.63 m/s²), and an escape velocity of 28.2 km/s.
In its orbital architecture around TOI-1472, TOI-1472 c completes one full revolution every 15.538 Earth days at a semi-major axis of 0.116 AU (orbiting interior to Mercury's 0.387 AU benchmark in the Solar System). Its mean orbital velocity is approximately 81.2 km/s (compared to Earth's 29.8 km/s). Its moderate orbital eccentricity of e = 0.172 carries the world between 0.096 AU at periapsis and 0.136 AU at apoapsis, driving measurable seasonal insolation cycles.
⚠️ Thermal Regime (Irradiated / Hot Zone): At an equilibrium temperature of 662 K (+389°C / +732°F) and receiving 32.77 S⊕ (~44,605 W/m²), TOI-1472 c orbits interior to the runaway greenhouse boundary where surface liquid water cannot persist.
The host star TOI-1472 is classified as a stellar host with an effective photospheric temperature of 5,100 K, a radius of 0.84 R☉, a mass of 0.87 M☉, an estimated bolometric luminosity of 0.428 L☉. Stellar evolution modeling indicates an estimated stellar age of 3.1 Gyr and a metallicity of [Fe/H] = 0.27 dex (metal-rich relative to the Sun). From Earth, TOI-1472 shines at apparent V-band magnitude 11.302 (faint and requiring research-grade or CCD telescopic photometry) in the Northern celestial hemisphere. The TOI-1472 system is a multi-planet architecture hosting 2 confirmed worlds, with TOI-1472 c sharing its stellar neighborhood alongside TOI-1472 b.
Methodology: Computed using the Schulze-Makuch et al. (2011) weighted metric comparing physical interior (radius, estimated density) and surface thermal regime (escape velocity, equilibrium temperature).
Discovery Facility: Multiple Observatories · Catalogue Source: NASA Exoplanet Archive (IPAC / Caltech).
☀️ Host Star Telemetry
| Host Star Name | TOI-1472 |
| Spectral Type | Unclassified |
| Effective Temp (Teff) | 5,100 K |
| Stellar Radius | 0.8400 R☉ |
| Stellar Mass | 0.8700 M☉ |
| Bolometric Luminosity | 0.428 L☉ |
| Metallicity [Fe/H] | 0.270 dex |
| Stellar Age | 3.100 Gyr |
| Apparent Magnitude | V: 11.302 · G: 11.111 |
| System Architecture | 1 Star, 2 Planets |
🪐 Orbital & Physical Dynamics
| Semi-Major Axis (a) | 0.116000 AU |
| Orbital Period | 15.538 days |
| Mean Orbital Velocity | 81.2 km/s |
| Orbital Eccentricity (e) | 0.17200 |
| Orbital Inclination (i) | 88.9060° |
| Mean Bulk Density | 3.14 g/cm³ (28.2 km/s vesc) |
| Insolation Flux | 32.7735 S⊕ (~44,605 W/m²) |
| Habitable Zone Status | Exterior / Non-HZ |
| Celestial Distance | 397.400 LY (121.840 pc) |