Kepler-93b
Super-Earth exoplanet in constellation Lyra
Kepler-93b (KOI-69b) is a hot, dense transiting Super-Earth exoplanet located approximately 313 light-years (96 parsecs)[4] away in the constellation of Lyra,[5][6] orbiting the G-type star[5] Kepler-93. Its discovery was announced in February 2014 by American astronomer Geoffrey Marcy and his team.[1] In July 2014, its radius was determined with a mere 1.3% margin of error, the most precise measurement ever made for an exoplanet's radius at the time.[7]
Physical properties
The planet has a radius of around 1.478 R🜨 (9,416 km), with an uncertainty of just 0.019 R🜨 (121 km),[8] making it the most precisely measured exoplanet ever in terms of radius as of July 2014.[7] The planet is substantially denser than Earth at 6.88±1.18 g/cm3[9] thanks to its high mass of roughly 4 ME, consistent with a rocky composition of iron and magnesium silicate.[9]
Based on these findings, the interior of the planet is likely similar to that of Earth and Venus, with an iron core making up around 26% of its total mass (albeit with a large uncertainty of ±20%),[10] compared to the 32.5 ± 0.1% of Earth and 31 ± 1% of Venus.[10]
The planet orbits its host star every 4.73 days[8] at a distance of 0.053 AU (7,900,000 km),[9] less than one-seventh the radius of Mercury's orbit. Its equilibrium temperature is approximately 1,133 K (860 °C; 1,580 °F),[3] which is as hot as lava and well above the melting point of aluminium.[a]
Host star
The planet orbits a Sun-like (spectral type G5V)[5] star named Kepler-93. The star has a mass of 0.911 M☉ and a radius of 0.919 R☉. It has a temperature of 5,669 K (5,396 °C; 9,745 °F) and is 6.6 billion years old.[8] In comparison, the Sun is 4.6 billion years old,[13] has a temperature of 5,772 K (5,499 °C; 9,930 °F) and a spectral type of G2V.[14] The apparent magnitude of the star is 9.931,[9] making it too dim to be visible from Earth by the naked eye.[15]
The star is host to an additional non-transiting confirmed companion, Kepler-93c, which was discovered using the radial-velocity method and announced in 2014, concurrently with Kepler-93b.[1] The object is most likely a brown dwarf orbiting much farther out than Kepler-93b, though its precise nature remains uncertain. The discovery paper reported a lower limit on the mass of 3 MJ and a minimal orbital period of 1,460 days (4.0 years),[1] while a subsequent study in 2015 weighed the planet at >8.5 MJ and presented an orbital period of >10 years, placing its orbit beyond 4.5 AU from the star,[9] and a 2023 study increased these lower limits further, to a mass >21 MJ, an orbital period >48.6 years, and a semi-major axis >13 AU.[3]
See also
- List of exoplanets discovered by the Kepler space telescope
- List of transiting exoplanets
- Other dense super-Earths orbiting close to their parent stars:
- CoRoT-7b, has a similar radius to Kepler-93b, but is more massive and much hotter.
- HD 219134 b, has a similar radius, mass and temperature.
- Kepler-10b, has a similar radius, but is slightly less massive and much hotter.
- Kepler-36b, has a similar radius, mass and temperature.
Footnotes
References
- ^ a b c d Marcy, Geoffrey W.; et al. (February 2014). "Masses, Radii, and Orbits of Small Kepler Planets: The Transition from Gaseous to Rocky Planets". The Astrophysical Journal Supplement Series. 210 (2): 20. arXiv:1401.4195. Bibcode:2014ApJS..210...20M. doi:10.1088/0067-0049/210/2/20. hdl:1721.1/92945. S2CID 10760418.
- ^ "The Extrasolar Planet Encyclopaedia — Kepler-93b". Extrasolar Planets Encyclopaedia. Retrieved 2024-05-04.
- ^ a b c d Bonomo, A. S.; Dumusque, X.; et al. (September 2023). "Cold Jupiters and improved masses in 38 Kepler and K2 small planet systems from 3661 HARPS-N radial velocities. No excess of cold Jupiters in small planet systems". Astronomy & Astrophysics. 677: A33. arXiv:2304.05773. Bibcode:2023A&A...677A..33B. doi:10.1051/0004-6361/202346211. S2CID 258078829.
- ^ Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c "BD+38 3853". SIMBAD. Retrieved 2024-05-08.
- ^ "SKY-MAP.ORG - Interactive Sky Map". Sky-Map.org. Retrieved 2024-05-08.
- ^ a b "Gauging an Alien World's Size". NASA. 2014-07-22. Retrieved 2024-05-07.
- ^ a b c Ballard, Sarah; et al. (July 2014). "Kepler-93b: A Terrestrial World Measured to within 120 km, and a Test Case for a New Spitzer Observing Mode". The Astrophysical Journal. 790 (1). arXiv:1405.3659. Bibcode:2014ApJ...790...12B. doi:10.1088/0004-637X/790/1/12. S2CID 12644226. 12.
- ^ a b c d e Dressing, Courtney D.; et al. (February 2015). "The Mass of Kepler-93b and The Composition of Terrestrial Planets". The Astrophysical Journal. 800 (2). arXiv:1412.8687. Bibcode:2015ApJ...800..135D. doi:10.1088/0004-637X/800/2/135. S2CID 53471038. 135.
- ^ a b Li, Zeng; et al. (March 2016). "Mass-Radius Relation for Rocky Planets based on PREM". The Astrophysical Journal. 819 (2). arXiv:1512.08827. Bibcode:2016ApJ...819..127Z. doi:10.3847/0004-637X/819/2/127. S2CID 119111854. 127.
- ^ Philpotts, Anthony R.; Ague, Jay J. (2009). Principles of igneous and metamorphic petrology (2nd ed.). Cambridge, UK: Cambridge University Press. pp. 53–55. ISBN 9780521880060.
- ^ "Technical data for the element Aluminum in the Periodic Table". The Photographic Periodic Table of the Elements. Retrieved 2024-05-31.
- ^ Connelly, JN; Bizzarro, M; Krot, AN; Nordlund, Å; Wielandt, D; Ivanova, MA (2 November 2012). "The Absolute Chronology and Thermal Processing of Solids in the Solar Protoplanetary Disk". Science. 338 (6107): 651–655. Bibcode:2012Sci...338..651C. doi:10.1126/science.1226919. PMID 23118187. S2CID 21965292.(registration required)
- ^ Williams, D.R. (1 July 2013). "Sun Fact Sheet". NASA Goddard Space Flight Center. Archived from the original on 2010-07-15. Retrieved 2013-08-12.
- ^ John E. Bortle (February 2001). "The Bortle Dark-Sky Scale". Sky & Telescope. Archived from the original on 2009-03-23. Retrieved 2009-11-18.
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