astro.wikisort.org - Meteorite

Kepler-10b is the first confirmed terrestrial planet to have been discovered outside the Solar System by the Kepler Space Telescope.[6] Discovered after several months of data collection during the course of the NASA-directed Kepler Mission, which aims to discover Earth-like planets crossing in front of their host stars, the planet's discovery was announced on January 10, 2011. Kepler-10b has a mass of 3.72±0.42 Earth masses and a radius of 1.47 Earth radii. However, it lies extremely close to its star, Kepler-10, and as a result is too hot to support life as we know it. Its existence was confirmed using measurements from the W.M. Keck Observatory in Hawaii.

Kepler-10b

Size comparison of Kepler-10b with Earth
Discovery[1]
Discovered by	Batalha et al.
Discovery date	January 10, 2011
Detection method	Transit (Kepler Mission)
Orbital characteristics
Semi-major axis	0.01684 +0.00032 −0.00034[1] AU
Eccentricity	0[1]
Orbital period (sidereal)	0.837495[1] d 20.0999 h
Inclination	84.4[1]
Semi-amplitude	3.3 +0.8 −1.0[1]
Star	Kepler-10[2]
Physical characteristics
Mean radius	1.47+0.03 −0.02[3] REarth
Mass	3.72±0.42[4] MEarth
Mean density	6.46±0.73 g/cm3[4]
Surface gravity	15 m/s2 (49 ft/s2)[3]
Albedo	0.5
Temperature	1,833 K (1,560 °C; 2,840 °F) (day side) 50 K (−223.2 °C; −369.7 °F) (night side)[5]

Nomenclature and history

Kepler-10, the star that hosts Kepler-10b, is located 560 light-years from the Solar System in the Draco constellation. It is approximately the same size as the Sun, with an estimated age of 12 billion years.[7] Planet Kepler-10b was the first planet to be discovered in the orbit of its star. For this, it was designated the star's b planet. The star, in turn, was named for the Kepler Mission, a NASA-led operation aimed at discovering terrestrial planets that transit, or cross in front of, their host stars with respect to Earth.[8] The planet's discovery was announced to the public on January 10, 2011.[9]

The transit method of discovering exoplanets relies upon carefully monitoring the brightness of a star. If a planet is present and crosses the line of sight between Earth and the star, the star will dim at a regular interval by an amount that depends upon the radius of the transiting planet. In order to measure the mass of a planet, and rule out other phenomena that can mimic the presence of a planet transiting a star, candidate transiting planets are followed up with the radial velocity method of detecting extrasolar planets.[10]

Kepler-10b's discovery was based on eight months of data collected with the Kepler telescope from May 2009 to January 2010. The planet's first transits were observed in July 2009. According to the collected data, Kepler-10 dimmed by one part in ten thousand every 0.83 days.[11][12] Kepler-10 was the first star in the field of view of the Kepler telescope identified as capable of harboring a small transiting planet, and was considered a high priority target for ground-based radial velocity observations intended to confirm the mass of Kepler-10b. Radial velocity measurements with the Keck I telescope taken intermittently between August 2009 and August 2010 revealed a periodic Doppler shift in the spectrum of Kepler-10 consistent with a planet of the nature observed by Kepler, confirming the planet's existence and allowing its mass to be determined.[1][11] The planet's discovery was announced to the public on January 10, 2011.[9]

In September 2011, the detection of secondary transit and phases were announced. This allowed to determine the temperature and albedo of the planet. This is the first terrestrial exoplanet with observed phases. Detection of phases was possible due to extreme day/night side temperature variations and the amount of starlight the planet receives due to its proximity to the host star.[13]

Reaction

Kepler-10b's discovery excited astronomers, who hoped to use data about it to inquire into the formation and structure that terrestrial, Earth-size planets tend to have in common.[14] Diana Valencia at the University of Côte d'Azur in Nice, France considered the planet more of a "super-Mercury" than a super-Earth, granted its physical characteristics.[15]

Characteristics

Kepler-10b is most noted for its rocky surface. It has a diameter 1.47 times that of the Earth.[3] The mass of Kepler-10b is 3.72±0.42 times that of Earth and the average density is 6.46±0.73 g cm⁻³.[4] It orbits its star, Kepler-10, in less than a day, at less than a twentieth of the distance from Mercury to the Sun. Its surface temperature on the star lit side is approximately 1833 K,[16] which is as hot as a blast furnace and hot enough to melt iron.[12]

Though CoRoT-7b was discovered before Kepler-10b and has been claimed to be rocky, there is more room for other interpretations in the case of CoRoT-7b's composition than there is for Kepler-10b.[12] This is due to the much larger uncertainty in CoRoT-7b's mass (and, to a lesser extent, its radius) which is illustrated in the plot to the left. Consequently, CoRoT-7b may be revealed to be a lava-ocean planet,^{[clarification needed]} whereas Kepler-10b must be predominantly made of rock or iron. In addition to showing the range of masses and radii consistent with the observations of each planet, the plot includes curves of compositions implied by certain masses and radii.

Kepler-10b is tidally locked to its parent star and has extreme variations in temperature between day and night sides. It also reflects about half of the starlight it receives. One possible explanation for the high Bond albedo could be that Kepler-10b is a coreless rocky planet with surface magma oceans rich in iron oxides.[17]

See also

• Kepler-10c
• Kepler Mission
• Kepler-4b, 5b, 6b, 7b, 8b, 9b, 78b
• List of exoplanet extremes

References

External links

Media related to Kepler-10 b at Wikimedia Commons

• NASA Kepler Mission (Kepler Discoveries): Kepler-10b
• YouTube: Narrated Animation on Kepler-10b

Preceded by Earth	Most dense planet 2011	Succeeded by PSR J1719-1438 b
Preceded by	Most dense exoplanet 2011	Succeeded by PSR J1719-1438 b

На других языках

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[de] Kepler-10b

Kepler-10b ist ein etwa erdgroßer Planet und umkreist Kepler-10 im Sternbild Drache am Nordhimmel. Er ist der erste Gesteinsplanet, der mithilfe des Weltraumteleskops Kepler entdeckt wurde. Der Exoplanet hat etwa die 1,47-fache Größe und 3,72-fache Masse der Erde[1] und war bis Januar 2011 der kleinste Planet, der bei einem anderen Stern aufgespürt und dessen Durchmesser mit der Transitmethode bestimmt werden konnte.[2] Er umrundet seinen Zentralstern Kepler-10, der 560 Lichtjahre von unserem Sonnensystem entfernt ist, etwa alle 0,84 Tage bei weniger als einem 20stel der Entfernung zwischen Merkur und Sonne.[3] Im gleichen System befindet sich auch Kepler-10c, ein größerer Gesteinsplanet, der den Stern alle 45 Tage umkreist.[4]

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- [en] Kepler-10b

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[ru] Kepler-10 b

Kepler-10 b — одна из экзопланет, открытых телескопом «Кеплер», по состоянию на январь 2011 года, была наименьшей экзопланетой (по радиусу)[3][4][5]. Судя по плотности (8,8 г/см³), это также первая достоверно известная железная экзопланета[5]. Изучение продолжалось восемь месяцев с мая 2009 до начала 2010 года[6]. Размером Kepler-10 b превосходит Землю всего в 1,4 раза[5], а обращается она вокруг своего светила за 0,84 земных суток, на расстоянии около 1/20 от радиуса орбиты Меркурия. Масса небесного тела составляет 4,5 массы нашей планеты[5].

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