LHS 3844 b
 Artist’s illustration of LHS 3844 b | |
| Discovery[1] | |
|---|---|
| Discovered by | Vanderspek et al. |
| Discovery date | September 2018 |
| Transit | |
| Designations | |
| Kua'kua,[2] TOI-136.01, TIC 410153553 b[3][4] | |
| Orbital characteristics | |
| 0.00622±0.00017 AU[3][4] | |
| 0.46292913±0.00000190 d[3][4] | |
| Inclination | 88.50±0.51[4] |
| Star | LHS 3844 |
| Physical characteristics | |
| 1.303±0.022 R🜨[3][4] | |
| Albedo | <0.2[5] |
| Temperature | 1,040 K (770 °C; 1,410 °F) (day side)[5] |
LHS 3844 b, formally named Kua'kua[pronunciation?],[2] is an exoplanet orbiting the red dwarf LHS 3844, about 48.5 light-years (14.9 parsecs) away in the constellation Indus,[6] discovered using the Transiting Exoplanet Survey Satellite. It orbits its parent star once every 11 hours, and its radius is 1.32 times that of Earth.[1] It has a low albedo, indicating that its surface may resemble that of the Moon or Mercury. LHS 3844 b probably does not have an atmosphere as almost no heat goes to its night side, and it has a dayside temperature of 1,040 K (770 °C; 1,410 °F).[5][7] The presence of cloudy atmosphere with cloud tops above pressure level of 0.1 bar cannot be excluded though.[8]
In order to explain the lack of atmosphere, it has been proposed that the planet was formed interior to the star system's snow-line, because if it formed beyond the snow-line it would have carried volatiles, on the surface and in a thick atmosphere, that according to models on atmospheric loss should have been enough to sustain an atmosphere to the present.[9] The planet probably also formed with a volatile-poor outgassing mantle, in a stagnant lid regime, because if the mantle was similar in constitution to Earth's, with plate tectonics, then it should still have a thick atmosphere, unless the red dwarf consistently flared at an uncharacteristically extreme rate not yet considered in atmospheric loss models.[9] An alternative explanation for the lack of atmosphere could be through a large impact event, one with enough momentum to strip the planet of its atmosphere and a large portion of its mantle.[9] In order to explain the non-replenishment of volatiles via comets back onto the planet, it is also proposed that perhaps there is an outer gas giant in the star system.[9]
It is thought that LHS 3844 b is tidally locked due to its surface being 'relatively cool', although this hypothesis could possibly be complicated by the fact that the research into the temperature of the planet assumed that there was no atmosphere, a point which is not definitively confirmed.[10]
Naming
In August 2022, this planet and its host star were included among 20 systems to be named by the third NameExoWorlds project.[6] The approved names, proposed by a team from Costa Rica, were announced in June 2023. LHS 3844 b is named Kua'kua and its host star is named Batsũ̀, after the Bribri words for "butterfly" and "hummingbird".[2]
See also
References
- ^ a b Team, the TESS; Villaseñor, Jesus Noel S.; Twicken, Joseph D.; Rose, Mark; Morgan, Edward H.; Pepper, Joshua; Glidden, Ana W.; Fausnaugh, Michael; Davies, Misty D. (2018-09-19). "TESS Discovery of an ultra-short-period planet around the nearby M dwarf LHS 3844". The Astrophysical Journal. 871 (2): L24. arXiv:1809.07242. Bibcode:2019ApJ...871L..24V. doi:10.3847/2041-8213/aafb7a. S2CID 119009146.
- ^ a b c "2022 Approved Names". nameexoworlds.iau.org. IAU. Retrieved 7 June 2023.
- ^ a b c d "The Extrasolar Planet Encyclopaedia — LHS 3844 b". Extrasolar Planets Encyclopaedia. 1995. Retrieved 2019-08-25.
- ^ a b c d e "LHS 3844 b". NASA Exoplanet Archive. Retrieved 23 July 2020.
- ^ a b c Kreidburg, Laura; et al. (August 2019). "Absence of a thick atmosphere on the terrestrial exoplanet LHS 3844b". Nature. 573 (7772): 87–90. arXiv:1908.06834. Bibcode:2019Natur.573...87K. doi:10.1038/s41586-019-1497-4. PMID 31427764. S2CID 256819677.
- ^ a b "List of ExoWorlds 2022". nameexoworlds.iau.org. IAU. 8 August 2022. Retrieved 27 August 2022.
- ^ Greicius, Tony (2019-08-19). "NASA Gets a Rare Look at a Rocky Exoplanet's Surface". NASA. Retrieved 2019-08-25.
- ^ Diamond-Lowe, Hannah; Charbonneau, David; Malik, Matej; Kempton, Eliza M.-R.; Beletsky, Yuri (2020), "Optical Transmission Spectroscopy of the Terrestrial Exoplanet LHS 3844b from 13 Ground-based Transit Observations", The Astronomical Journal, 160 (4): 188, arXiv:2008.05444, Bibcode:2020AJ....160..188D, doi:10.3847/1538-3881/abaf4f, S2CID 221103928
- ^ a b c d Kane, Stephen R.; Roettenbacher, Rachael M.; Unterborn, Cayman T.; Foley, Bradford J.; Hill, Michelle L. (2020-07-28). "A Volatile-poor Formation of LHS 3844b Based on Its Lack of Significant Atmosphere". The Planetary Science Journal. 1 (2): 36. arXiv:2007.14493. Bibcode:2020PSJ.....1...36K. doi:10.3847/PSJ/abaab5. S2CID 220845575.Accepted for publication in the Planetary Science Journal
- ^ Howlett, Joseph (2024-03-28). "This super-Earth is the first planet confirmed to have a permanent dark side". Nature. doi:10.1038/d41586-024-00414-z.
