TOI-1130 b
Astrophysical Synthesis & Habitability Characterization
TOI-1130 b is a confirmed sub-neptune exoplanet orbiting the star TOI-1130, located approximately 190 light-years (58.26 parsecs) from the Solar System. First announced in 2020 by Transiting Exoplanet Survey Satellite (TESS) using the Transit detection technique (producing an estimated primary transit depth of 0.2318% across the stellar disk), this world measures 3.66 Earth radii (0.33 Jupiter radii) and has a measured mass of 19.8 Earth masses. Combining its mass and radius yields a mean bulk density of 2.23 g/cm³ (an intermediate density indicative of a deep water-ice mantle or dense volatile envelope), a surface gravity of 1.48 g⊕ (14.51 m/s²), and an escape velocity of 26 km/s.
In its orbital architecture around TOI-1130, TOI-1130 b completes one full revolution every 4.075 Earth days at a semi-major axis of 0.0453 AU (an ultra-close orbit less than one-seventh of Mercury's 0.387 AU distance from the Sun, where strong stellar tidal forces typically induce synchronous rotation). Its mean orbital velocity is approximately 121 km/s (compared to Earth's 29.8 km/s). Its moderate orbital eccentricity of e = 0.05216 carries the world between 0.0429 AU at periapsis and 0.0477 AU at apoapsis, driving measurable seasonal insolation cycles.
⚠️ Thermal Regime (Irradiated / Hot Zone): At an equilibrium temperature of 825 K (+552°C / +1026°F) and receiving 78.10 S⊕ (~106,294 W/m²), TOI-1130 b orbits interior to the runaway greenhouse boundary where surface liquid water cannot persist.
The host star TOI-1130 is classified as an orange K-type star of spectral type K6-K7 with an effective photospheric temperature of 4,360 K, a radius of 0.697 R☉, a mass of 0.745 M☉, an estimated bolometric luminosity of 0.158 L☉. Stellar evolution modeling indicates an estimated stellar age of 5.4 Gyr and a metallicity of [Fe/H] = 0.11 dex (metal-rich relative to the Sun). From Earth, TOI-1130 shines at apparent V-band magnitude 11.595 (faint and requiring research-grade or CCD telescopic photometry) in the Southern celestial hemisphere. The TOI-1130 system is a multi-planet architecture hosting 2 confirmed worlds, with TOI-1130 b sharing its stellar neighborhood alongside TOI-1130 c.
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: Transiting Exoplanet Survey Satellite (TESS) · Catalogue Source: NASA Exoplanet Archive (IPAC / Caltech).
☀️ Host Star Telemetry
| Host Star Name | TOI-1130 |
| Spectral Type | K6-K7 |
| Effective Temp (Teff) | 4,360 K |
| Stellar Radius | 0.6970 R☉ |
| Stellar Mass | 0.7450 M☉ |
| Bolometric Luminosity | 0.158 L☉ |
| Metallicity [Fe/H] | 0.110 dex |
| Stellar Age | 5.400 Gyr |
| Apparent Magnitude | V: 11.595 · G: 10.903 |
| System Architecture | 1 Star, 2 Planets |
🪐 Orbital & Physical Dynamics
| Semi-Major Axis (a) | 0.045300 AU |
| Orbital Period | 4.075 days |
| Mean Orbital Velocity | 121 km/s |
| Orbital Eccentricity (e) | 0.05216 |
| Orbital Inclination (i) | 87.4900° |
| Mean Bulk Density | 2.23 g/cm³ (26 km/s vesc) |
| Insolation Flux | 78.1000 S⊕ (~106,294 W/m²) |
| Habitable Zone Status | Exterior / Non-HZ |
| Celestial Distance | 190.000 LY (58.261 pc) |