astro.wikisort.org - Meteorite

K2-22b (also known as EPIC 201637175 b) is an exoplanet 801 ly from Earth, rapidly orbiting the red dwarf K2-22 with an orbital period of 9.145872 hours.[2] It has a mass below 445 M_e and a radius below 2.5 R_e. The planet was not detected in the K2 photometry. K2 photometry reveals the presence of an anomalous light curve consistent with evaporation of dust from the planet. This dust forms a tail both ahead and behind the planet, similar to some comets in the Solar System.[1] The evaporation of this dust requires a low surface gravity from the host planet, implying it is a low mass, "Mars, Mercury, or even lunar sized bodies with surface gravities of 1/6 to 1/3 that of Earth are to be preferred."[1]

K2-22b

Discovery[1]
Discovery site	Kepler Space Observatory
Discovery date	2015
Detection method	Transit
Orbital characteristics
Semi-major axis	0.0088 AU (1,320,000 km)
Eccentricity	null[2]
Orbital period (sidereal)	0.381078[2] d
Inclination	null[2]
Star	K2-22
Physical characteristics
Mean radius	<0.71REarth[3]
Mass	0.02 MEarth[3]
Temperature	2,100 K (1,830 °C; 3,320 °F)

The survey in 2020 has failed to validate the existence of the planet, although did not claim it to be a false positive.[4]

The observation of planetary system in 2021 has failed to detect the planet itself, placing an upper limit of 0.71R_Earth on its size. With the observed mass loss rate, the probable planet mass is 0.02M_Earth, and the planet will be gone in 21 million years in future.[3]

See also

•  Astronomy portal
• List of exoplanet extremes

References

На других языках

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- [en] K2-22b

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[es] K2-22b

K2-22b (también conocido como EPIC 201637175 b [1]) es un exoplaneta 801 años luz de la Tierra, orbitando rápidamente a la enana roja K2-22 con un período orbital de 9.145872 horas. Tiene una masa inferior a 445 de la masa terrestre y un radio inferior a 2.5 del radio terrestre. La fotometría K2 revela la presencia de una curva de luz anómala consistente con la evaporación del polvo del planeta. Este polvo forma una cola tanto delante como detrás del planeta, similar a algunos cometas del Sistema Solar. La evaporación de este polvo requiere una baja gravedad de la superficie del planeta anfitrión, lo que implica que es una masa baja, "Marte, Mercurio, o incluso cuerpos de tamaño lunar con gravedad de 1/6 a 1/3 de la Tierra son preferibles". Este polvo puede estar relacionado con el acercamiento del planeta al límite de Roche impuesto por la estrella, comenzando esta última a quitarle su atmósfera para luego desintegrarlo (Ridden-Harper et al. 2019).

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