Gliese 581e

Gliese 581e /ˈɡliːzə/ or Gl 581e is an exoplanet orbiting within the Gliese 581 system, located 20.5 light-years (6.3 parsecs) away from Earth in the Libra constellation. It is the third planet discovered in the system (fourth if the disputed planet candidate Gliese 581d is included) and the first in order from the star.

Gliese 581e

Size comparison of Gliese 581e with Earth (Based on selected hypothetical modeled compositions)[a]
Discovery[1]
Discovered by	Mayor et al.
Discovery site	La Silla Observatory, Chile
Discovery date	21 April 2009
Detection method	Radial velocity
Orbital characteristics[2]
Semi-major axis	0.02799±0.0003 AU
Eccentricity	0.012+0.015 −0.008
Orbital period (sidereal)	3.1481±0.0004 d
Inclination	47°+15° −13°
Time of periastron	2454752.33 ± 0.05[3]
Argument of periastron	226°+91° −55°
Semi-amplitude	1.8±0.1 m/s
Star	Gliese 581
Physical characteristics[2]
Mass	2.48+0.70 −0.42 M🜨

The planet was discovered by an Observatory of Geneva team led by Michel Mayor, using the HARPS instrument on the European Southern Observatory 3.6 m (140 in) telescope in La Silla, Chile. The discovery was announced on 21 April 2009. Mayor's team employed the radial velocity technique, in which the orbit size and mass of a planet are determined based on the small perturbations it induces in its parent star's orbit via gravity.^[1]

With a minimum mass of about 1.9 Earth masses, Gliese 581e was the least massive exoplanet known around a normal star at the time of discovery in 2009, with only PSR B1257+12 A being less massive.^[4][5] A 2024 study determined the orbital inclination of the planet, allowing its true mass to be determined, which is about 30% greater than the minimum mass at about 2.5 Earth masses.^[2]

Gliese 581e completes an orbit around its parent star in 3.15 days. At an orbital distance of just 0.028 AU (4,200,000 km) from its parent star, it orbits further in than the habitable zone.^[3] Although scientists think it probably has a rocky surface similar to Earth, it is also likely to experience intense tidal heating similar to (and likely more intense than) that affecting Jupiter's moon Io.^[6]

See also

• Habitability of red dwarf systems

Notes

1. The estimated range of sizes in this image from 2009 is based on the planet's minimum mass. Since the true mass is now known to be somewhat greater, the sizes may be underestimated.