TOI-5292 A b
Astrophysical Synthesis & Habitability Characterization
TOI-5292 A b is a confirmed gas giant exoplanet orbiting the star TOI-5292 A, located approximately 1099.5 light-years (337.1 parsecs) from the Solar System. First announced in 2026 by Transiting Exoplanet Survey Satellite (TESS) using the Transit detection technique (producing an estimated primary transit depth of 3.5994% across the stellar disk), this world measures 12.644 Earth radii (1.13 Jupiter radii) and has a measured mass of 412.859 Earth masses (1.3 Jupiter masses). Combining its mass and radius yields a mean bulk density of 1.13 g/cm³ (a low bulk density dominated by an extended hydrogen-helium gaseous envelope), a surface gravity of 2.58 g⊕ (25.3 m/s²), and an escape velocity of 63.9 km/s.
In its orbital architecture around TOI-5292 A, TOI-5292 A b completes one full revolution every 2.022 Earth days at a semi-major axis of 0.0279 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 150.1 km/s (compared to Earth's 29.8 km/s). With a near-circular eccentricity of e = 0.034 (ranging from 0.027 AU at periapsis to 0.0288 AU at apoapsis), the planet experiences minimal orbital distance variation.
⚠️ Thermal Regime (Irradiated / Hot Zone): At an equilibrium temperature of 809 K (+536°C / +997°F) and receiving 102.00 S⊕ (~138,822 W/m²), TOI-5292 A b orbits interior to the runaway greenhouse boundary where surface liquid water cannot persist.
The host star TOI-5292 A is classified as a low-mass red dwarf of spectral type M0±0.5 with an effective photospheric temperature of 3,919 K, a radius of 0.611 R☉, a mass of 0.596 M☉, an estimated bolometric luminosity of 0.079 L☉. Stellar evolution modeling indicates an estimated stellar age of 5 Gyr and a metallicity of [Fe/H] = 0.33 dex (metal-rich relative to the Sun). From Earth, TOI-5292 A shines at apparent V-band magnitude 16.416 (faint and requiring research-grade or CCD telescopic photometry) in the Southern celestial hemisphere.
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-5292 A |
| Spectral Type | M0±0.5 |
| Effective Temp (Teff) | 3,919 K |
| Stellar Radius | 0.6110 R☉ |
| Stellar Mass | 0.5960 M☉ |
| Bolometric Luminosity | 0.079 L☉ |
| Metallicity [Fe/H] | 0.330 dex |
| Stellar Age | 5.000 Gyr |
| Apparent Magnitude | V: 16.416 · G: 15.909 |
| System Architecture | 2 Stars, 1 Planet |
🪐 Orbital & Physical Dynamics
| Semi-Major Axis (a) | 0.027900 AU |
| Orbital Period | 2.022 days |
| Mean Orbital Velocity | 150.1 km/s |
| Orbital Eccentricity (e) | 0.03400 |
| Orbital Inclination (i) | 88.8700° |
| Mean Bulk Density | 1.13 g/cm³ (63.9 km/s vesc) |
| Insolation Flux | 102.0000 S⊕ (~138,822 W/m²) |
| Habitable Zone Status | Exterior / Non-HZ |
| Celestial Distance | 1099.500 LY (337.095 pc) |