HD 125595 b

Astrophysical Synthesis & Habitability Characterization

HD 125595 b is a confirmed gas giant exoplanet orbiting the star HD 125595, located approximately 92 light-years (28.2 parsecs) from the Solar System. First announced in 2011 by La Silla Observatory using the Radial Velocity detection technique (measuring periodic Doppler reflex motion in the host star's spectrum), this world has a minimum or true mass of 3531.074 Earth masses (11.11 M♃), while its physical transit radius has not yet been geometrically observed.

In its orbital architecture around HD 125595, HD 125595 b completes one full revolution every 9.674 Earth days at a semi-major axis of 0.08 AU (orbiting interior to Mercury's 0.387 AU benchmark in the Solar System). Its mean orbital velocity is approximately 90 km/s (compared to Earth's 29.8 km/s). The orbit is modeled as circular (e = 0.00), maintaining a constant stellar distance throughout its year.

⚠️ Thermal Regime (Irradiated / Hot Zone): At an equilibrium temperature of 688 K (+415°C / +779°F) and receiving 37.71 S⊕ (~51,321 W/m²), HD 125595 b orbits interior to the runaway greenhouse boundary where surface liquid water cannot persist.

The host star HD 125595 is classified as an orange K-type star of spectral type K4 V with an effective photospheric temperature of 4,691 K, a radius of 0.74 R☉, a mass of 0.29 M☉, an estimated bolometric luminosity of 0.238 L☉. Stellar evolution modeling indicates an estimated stellar age of 3.53 Gyr and a metallicity of [Fe/H] = 0.08 dex (metal-rich relative to the Sun). From Earth, HD 125595 shines at apparent V-band magnitude 9.03 (accessible to binoculars and small amateur telescopes) in the Southern celestial hemisphere.

Discovery Facility: La Silla Observatory · Catalogue Source: NASA Exoplanet Archive (IPAC / Caltech).