Kepler-62b

transit method, in which the dimming effect that a planet causes as it crosses in front of its star is measured. It is likely to have an equilibrium temperature slightly higher than the surface temperature of Venus (around 750 K (477 °C; 890 °F)), high enough to melt some types of metal.^[1] Its stellar flux is 70 ± 9 times Earth's.^[1]

equilibrium temperature of 750 K (477 °C; 890 °F). This is hot enough to melt some types of metal. It has a radius of 1.3 R_🜨,^[1] placing it below the estimated radius of ≤1.6 R_🜨 where it would otherwise be a mini-Neptune with a volatile composition, with no solid surface.^[2] However, the mass is currently not known, estimates place an upper limit of <9 M_E, the actual mass is expected to be significantly lower than this.^[1]

K and is 7 billion years old.^[1] In comparison, the Sun is 4.6 billion years old^[3] and has a surface temperature of 5778 K.^[4]

sunlight than Earth does from the Sun.^[1]

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-62; 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-62b occurred roughly every 5 days (its orbital period), it was eventually concluded that a planetary body was responsible for the periodic 5-day transits. The discovery, along with the planetary system of the star Kepler-69 were announced on April 18, 2013.^[1]