Kepler-69c

Physical characteristics

Mass, radius and temperature

Kepler-69c is a super-Earth, an exoplanet that has a radius and mass larger than Earth, but smaller than that of the ice giants Uranus and Neptune. It has an estimated equilibrium temperature of 325 K, but likely has a far hotter surface temperature of 548 K. It has an estimated mass of around 2.14 and a radius of 1.71 . These characteristics make it an analog to the planet Venus, but more massive, so it is called a "super-Venus".

Host star

Main article: Kepler-69

The planet orbits a (G-type) star named Kepler-69, orbited by a total of two planets. The star has a mass of 0.81 and a radius of 0.93 . and has a surface temperature of 5778 K.

The star's apparent magnitude, or how bright it appears from Earth's perspective, is 13.7. Therefore, Kepler-69 is too dim to be seen with the naked eye.

Orbit

Kepler-69c orbits its host star every 242 days at a distance of 0.64 times that of Earth. This is very similar to that of Venus's orbital period and distance in the Solar System.

Proposed habitability

The exoplanet, along with the exoplanets Kepler-62e and Kepler-62f, were announced in the media as being located within the star's "habitable zone", a region where liquid water could exist on the surface of the planet. It was described as being one of the most Earth-like planets, in terms of size and temperature yet found and, according to the scientists, a "prime candidate to host alien life".

Due to uncertainties in the stellar parameters, the error bars on the value of the incident flux on this planet are quite large, at 1.91 times the level of Earth. Using the nominal parameters, the planet is too close to the star to be habitable, though the uncertainties allow for the possibility that it may actually lie in the innermost region of the habitable zone and be a desert planet, however even with the lowest error bar measurement, a stellar flux of 1.35 S🜨 would still be high enough to boil away any oceans. A more recent analysis has shown that the planet is likely more analogous to Venus, which is known to be one of the most inhospitable places to life in the Solar System, and thus highly unlikely to be habitable to such organisms.

Discovery

In 2009, NASA's Kepler spacecraft was observing stars with its photometer, an instrument it uses to detect transit events, in which a planet crosses in front of and dims its host star for a brief and roughly regular period of time. In this last test, Kepler observed stars in the Kepler Input Catalog, including Kepler-69; the preliminary light curves were sent to the Kepler science team for analysis, who chose obvious planetary companions from the bunch for follow-up at observatories. Observations for the potential exoplanet candidates took place between 13 May 2009 and 17 March 2012. After observing the respective transits, which for Kepler-69c occurred roughly every 242 days (its orbital period), it was eventually concluded that a planetary body was responsible for the periodic 242-day transits. The discovery, along with the planetary system of the star Kepler-62 were announced on April 18, 2013.

On 9 May 2013, a congressional hearing by two U.S. House of Representatives subcommittees discussed "Exoplanet Discoveries: Have We Found Other Earths?," prompted by the discovery of exoplanet Kepler-69c, along with Kepler-62e and Kepler-62f. A related special issue of the journal Science, published earlier, described the discovery of the exoplanets.

References

Notes

References

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4. (3 May 2013). "Special Issue: Exoplanets". [[Science (journal).
5. Kane, Stephen. (2013). "A Potential Super-Venus in the Kepler-69 System". The Astrophysical Journal Letters.
6. Barclay, Thomas. (2013). "A super-Earth-sized planet orbiting in or near the habitable zone around Sun-like star". The Astrophysical Journal.
7. Staff. "NASA Exoplanet Archive -KOI-172.02". [[Caltech]].
8. (18 April 2013). "NASA's Kepler Discovers Its Smallest 'Habitable Zone' Planets to Date". [[NASA]].
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13. (2020-09-01). "The Gaia-Kepler Stellar Properties Catalog. II. Planet Radius Demographics as a Function of Stellar Mass and Age". The Astronomical Journal.