TOI-1470 b
Astrophysical Synthesis & Habitability Characterization
TOI-1470 b is a confirmed sub-neptune exoplanet orbiting the star TOI-1470, located approximately 169.4 light-years (51.95 parsecs) from the Solar System. First announced in 2023 by Transiting Exoplanet Survey Satellite (TESS) using the Transit detection technique (producing an estimated primary transit depth of 0.1816% across the stellar disk), this world measures 2.18 Earth radii and has a measured mass of 7.32 Earth masses. Combining its mass and radius yields a mean bulk density of 3.9 g/cm³ (an intermediate density indicative of a deep water-ice mantle or dense volatile envelope), a surface gravity of 1.54 g⊕ (15.1 m/s²), and an escape velocity of 20.5 km/s.
In its orbital architecture around TOI-1470, TOI-1470 b completes one full revolution every 2.527 Earth days at a semi-major axis of 0.0285 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 122.7 km/s (compared to Earth's 29.8 km/s). The planet follows a highly eccentric trajectory (e = 0.3, swinging from 0.02 AU at periapsis out to 0.0371 AU at apoapsis), pointing to past dynamical scattering or secular gravitational perturbations.
⚠️ Thermal Regime (Irradiated / Hot Zone): At an equilibrium temperature of 734 K (+461°C / +862°F) and receiving 46.30 S⊕ (~63,014 W/m²), TOI-1470 b orbits interior to the runaway greenhouse boundary where surface liquid water cannot persist.
The host star TOI-1470 is classified as a low-mass red dwarf of spectral type M1.5 V with an effective photospheric temperature of 3,709 K, a radius of 0.469 R☉, a mass of 0.471 M☉, an estimated bolometric luminosity of 0.037 L☉. Stellar evolution modeling indicates an estimated stellar age of 1.3 Gyr and a metallicity of [Fe/H] = 0 dex (near-solar heavy-element abundance). From Earth, TOI-1470 shines at apparent V-band magnitude 13.459 (faint and requiring research-grade or CCD telescopic photometry) in the Northern celestial hemisphere. The TOI-1470 system is a multi-planet architecture hosting 2 confirmed worlds, with TOI-1470 b sharing its stellar neighborhood alongside TOI-1470 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-1470 |
| Spectral Type | M1.5 V |
| Effective Temp (Teff) | 3,709 K |
| Stellar Radius | 0.4690 R☉ |
| Stellar Mass | 0.4710 M☉ |
| Bolometric Luminosity | 0.037 L☉ |
| Metallicity [Fe/H] | 0.000 dex |
| Stellar Age | 1.300 Gyr |
| Apparent Magnitude | V: 13.459 · G: 12.556 |
| System Architecture | 1 Star, 2 Planets |
🪐 Orbital & Physical Dynamics
| Semi-Major Axis (a) | 0.028500 AU |
| Orbital Period | 2.527 days |
| Mean Orbital Velocity | 122.7 km/s |
| Orbital Eccentricity (e) | 0.30000 |
| Orbital Inclination (i) | 87.4200° |
| Mean Bulk Density | 3.9 g/cm³ (20.5 km/s vesc) |
| Insolation Flux | 46.3000 S⊕ (~63,014 W/m²) |
| Habitable Zone Status | Exterior / Non-HZ |
| Celestial Distance | 169.400 LY (51.950 pc) |