The Kepler-327 system contains 3 exoplanets. It is located 789.26 light years away from the solar system.
Mass | 0.59 solar masses |
Radius | 0.49 solar radiae |
Temperature | 3799 kelvin |
Stellar Metallicity | -0.2 decimal exponent |
Age | 3.02 billion years |
At less than 1.5 Earth masses, Kepler-327 b is a terrestrial planet, much like the terrestrial planets we find in our solar system, namely Mercury, Venus, Earth and Mars.
Mass | 1.410 Earth masses |
Density | 5.670 grams per cubic centimeter |
Radius | 1.110 Earth radiae |
Semi-major Axis | 0.029 AU |
Eccentricity | 0 |
Orbital Period | 2.550 days |
Discovery Method | Transit |
Discovery Facility | Kepler |
Discovery Telescope | 0.95 m Kepler Telescope |
Discovery Instrument | Kepler CCD Array |
Discovery Date | 2014-03 |
Reference | Rowe et al. 2014 |
At more than 10 Earth masses, Kepler-327 c is an ice giant, a planet that is made up mostly of volatiles like water, amonia and methane, and enveloped by a dense hydrogen and helium atmosphere, much like Uranus and Neptune.
Mass | 20.300 Earth masses |
Density | 102.000 grams per cubic centimeter |
Radius | 1.030 Earth radiae |
Semi-major Axis | 0.047 AU |
Eccentricity | 0 |
Orbital Period | 5.212 days |
Discovery Method | Transit |
Discovery Facility | Kepler |
Discovery Telescope | 0.95 m Kepler Telescope |
Discovery Instrument | Kepler CCD Array |
Discovery Date | 2014-03 |
Reference | Rowe et al. 2014 |
At 3.657 Earth masses, Kepler-327 d is a so called Super Earth. Super Earths could be terrestrial worlds like Earth, but they could also be ocean worlds or terrestrial worlds wrapped in a substantial atmosphere, in which case some refer to them as Mini Neptunes.
Mass | 3.640 Earth masses |
Density | 3.860 grams per cubic centimeter |
Radius | 1.730 Earth radiae |
Semi-major Axis | 0.09 AU |
Eccentricity | 0 |
Orbital Period | 13.969 days |
Discovery Method | Transit |
Discovery Facility | Kepler |
Discovery Telescope | 0.95 m Kepler Telescope |
Discovery Instrument | Kepler CCD Array |
Discovery Date | 2014-03 |
Reference | Rowe et al. 2014 |