Kepler-62d

transit method, in which the dimming that a planet causes as it crosses in front of its star is measured.^[1] Its stellar flux is 15 ± 2 times Earth's.^[1] Due to its closer orbit to its star, it is a super-Venus or, if it has a volatile composition, a hot Neptune

equilibrium temperature of 510 K (237 °C; 458 °F). It has a radius of 1.95 R_🜨.^[1] Because of its radius (and temperature), it is likely to be either a "super-Venus", or a hot mini-Neptune, with no solid surface. However, the mass is currently not known, estimates place an upper limit of 14 M_E, the real mass is expected to be lower than this.^[1] The true value is likely around 5.5 M_E, based on its composition.^[2]

K and is 7 billion years old.^[1] In comparison, the Sun is 4.6 billion years old^[3] and has a temperature of 5778 K.^[4] The star is somewhat metal-poor, with a metallicity ([Fe/H]) of −0.37, or 42% of the solar amount.^[1] Its luminosity (L_☉) is 21% that of the Sun.^[1]

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