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<6 M[2][3][lower-alpha 1] kg

Kepler-37b is an extrasolar planet (exoplanet) orbiting Kepler-37 in the constellation Lyra.[4] Template:As of it is the smallest planet discovered around a main-sequence star, with a radius slightly greater than that of the Moon.[5] The measurements do not constrain its mass, but masses above a few times that of the Moon give unphysically high densities.[3]


File:A Moon-size Line Up.jpg

Kepler-37b, along with two other planets, Kepler-37c and Kepler-37d, were discovered by the Kepler space telescope, which observes stellar transits.[6][7] After observing transits of Kepler-37b, astronomers had to compare it with the size of the parent star.

The size of the star was obtained using asteroseismology;Template:Clarify[8] Kepler-37 is currently the smallest star to be studied using this process.[7] This allowed the size of Kepler-37b to be determined "with extreme accuracy".[7]

To date, Kepler-37b is the smallest planet discovered around a main-sequence star[lower-alpha 2] outside the Solar System.[5] Detection of Kepler-37b was possible due to its short orbital period, relative brightness, and low activity of its host star, allowing brightness data to average out quickly.[9] The discovery of Kepler-37b has led Jack Lissauer, a scientist at NASA's Ames Research Center, to conjecture that "such little planets are common".[7]



Kepler-37b is located approximately 210 light-years from Earth.[10] It is slightly larger than the Moon, with a diameter of about Script error.[8] NASA states that it probably has no atmosphere and cannot support life.[7] Furthermore, it is most likely composed of rocky materials.[7] Because it is so close to its star (Mercury is more than three times as far from the Sun), Kepler-37b's mean temperature is estimated to be around Script error.[7]


The innermost known planet in its system, Kepler-37b, orbits its parent star at a distance of about 15 million kilometers (9.3 million miles), with a period of roughly 13 days.[5] The outer two planets in the system have orbital periods[6][11] within one percent of the 8:5 and 3:1 resonances with Kepler-37b's period.

See alsoEdit




Template:S-start Template:S-ach Template:S-bef Template:S-ttl Template:S-aft Template:S-bef Template:S-ttl Template:S-aft Template:S-end

Template:Kepler-37 Template:Exoplanets Template:2013 in space

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