K2-148b is a confirmed super-Earth, probably rocky, closely orbiting a small orange dwarf star. It is the innermost of three Super-Earths around the star K2-148, which is in a wide binary pair with the M0.5V red dwarf EPIC 220194953. K2-148b is the smallest planet of the system, at about a third larger than Earth, and could be terrestrial in nature. However, the three planets do not exhibit significant transit timing variations, implying that they could have relatively low masses. The planet was validated in early 2018 by Hirano et al. and is too hot for known life.
 Size comparison of the planet K2-148b (artistic concept) with Earth | |
| Discovery | |
|---|---|
| Discovered by | Hirano et al. 2018 |
| Discovery date | 19 January 2018 |
| Transit | |
| Orbital characteristics | |
| 0.0454 (± 0.0014)[1] AU | |
| Eccentricity | null[1] |
| 4.38395 (± 0.00080)[1] d | |
| Inclination | null[1] |
| Star | K2-148 |
| Physical characteristics | |
| 1.33+0.19 −0.18[1] R🜨 | |
| Temperature | 674 K (401 °C; 754 °F)[2] |
Characteristics
editMass, radius, and temperature
editK2-148b is a Super-Earth, meaning that it is larger than Earth but smaller than the ice giants Uranus and Neptune. Because it was detected with the transit method, only the radius of the planet is known. It is 1.33 R🜨, about a third larger than Earth.[1] A planet of this size is likely rocky, and with an Earth-like composition, K2-148b would have a mass of about 2.5 ME. Since K2-148b is in a multiple planet system, transit timing variations could be used to determine the masses of the planets by seeing how the planets pull on each other and slightly change when they transit the star. However, the TTVs of the K2-148 system were quite low, which may mean that K2-148b is not rocky.[3]
The planet is quite hot due to its proximity to its host star, with an equilibrium temperature of 674 K (401 °C; 754 °F), far too high for liquid water to exist on its surface.[2] It receives about 48 times more sunlight than Earth gets from the Sun.[3]
Orbit
editK2-148b has a tight orbit around its host star. It only takes about 4.4 Earth days for the planet to complete one full orbit around its star, with a semi-major axis of 0.0454 AU. For comparison, the innermost planet in the Solar System, Mercury, takes 88 days to orbit at a distance of 0.38 AU. The eccentricity and inclination of K2-148b's orbit are currently unknown.[1]
Host star
editK2-148b orbits a late-K dwarf star known as K2-148, or EPIC 220194974. It is 63% the radius, 65% the mass, and 10% the luminosity of the Sun, with a temperature of 4079 K and an unknown age. For comparison, the Sun has a temperature of 5778 K and is 4.5 billion years old. It is orbited by a slightly smaller M0.5V red dwarf known as EPIC 220194953 at a distance of 1,100 AU. The companion star is about 58% the radius, 60% the mass, and 6.6% as luminous as the Sun with a temperature of 3854 K. EPIC 220194953 is slightly more metal-rich than K2-148, and the two are confirmed to be gravitationally bound to each other.[3]
See also
edit- Kepler-296e and Kepler-296f, two Super-Earths orbiting a red dwarf in a wide binary system. The two planets mark the inner and outer boundaries of the system's habitable zone.
References
edit- ^ a b c d e f g "K2-148 b CONFIRMED PLANET OVERVIEW PAGE". NASA Exoplanet Archive. Retrieved 2018-02-25.
- ^ a b "PHL's calculators". Archived from the original on 2021-10-18. Retrieved 2018-02-26.
- ^ a b c Hirano, Teruyuki; Dai, Fei; Gandolfi, Davide; Fukui, Akihiko; Livingston, John H.; Miyakawa, Kohei; Endl, Michael; Cochran, William D.; Alonso-Floriano, Francisco J.; Kuzuhara, Masayuki; Montes, David; Ryu, Tsuguru; Albrecht, Simon; Barragan, Oscar; Cabrera, Juan; Csizmadia, Szilard; Deeg, Hans; Eigmüller, Philipp; Erikson, Anders; Fridlund, Malcolm; Grziwa, Sascha; Guenther, Eike W.; Hatzes, Artie P.; Korth, Judith; Kudo, Tomoyuki; Kusakabe, Nobuhiko; Narita, Norio; Nespral, David; Nowak, Grzegorz; et al. (2018). "Exoplanets around Low-mass Stars Unveiled by K2". The Astronomical Journal. 155 (3): 127. arXiv:1710.03239. Bibcode:2018AJ....155..127H. doi:10.3847/1538-3881/aaa9c1. S2CID 54590874.