Kepler-69c

Kepler-69c (also known by its Kepler Object of Interest designation KOI-172.02) is a confirmed super-Earth extrasolar planet, likely rocky, orbiting the Sun-like star Kepler-69, the outermost of two such planets discovered by NASA's Kepler spacecraft. It is located about 2,430 light-years (746 parsecs) from Earth Kepler-69c (also known by its Kepler Object of Interest designation KOI-172.02) is a confirmed super-Earth extrasolar planet, likely rocky, orbiting the Sun-like star Kepler-69, the outermost of two such planets discovered by NASA's Kepler spacecraft. It is located about 2,430 light-years (746 parsecs) from Earth 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 a surface temperature of 548 K (275 °C; 527 °F). It has an estimated mass of around 6 M⊕, and a radius of 1.71 R⊕. These characteristics make it an analog to Venus, but more massive, so it is called a 'super-Venus'. 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 M☉ and a radius of 0.93 R☉. It has a surface temperatures of 5638 K and has an estimated age of around 400 million years, meaning it has probably finished planet formation. In comparison, the Sun is about 4.6 billion years old 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. Kepler-69c orbits its host star with about 80% of the Sun's luminosity 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. 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+0.43−0.56 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, 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. The planet would be inhospitable because of a runaway greenhouse effect on its surface. Any oceans on its surface would've boiled away due to the high stellar flux, and as this occurred, the temperature would've risen to around 322 K (49 °C; 120 °F). The water vapor would've accumulated in the atmosphere to the point where the surface temperature would rise to around 500 K (227 °C; 440 °F) as the planet would've been overwhelmed by water vapor (it is a powerful greenhouse gas). Little amounts of carbon dioxide would've been present, as Kepler-69c was probably an ocean planet (with little to no landmasses) very shortly after its star was born into the main sequence, before the stellar flux increased to its estimated present value. The surface pressure would've also increased to around 100 times Earth's surface pressure (100 kilopascals, 100 atm.) because of the amount of water vapor in the atmosphere. 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 50000 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.