Kepler-93b

Last updated
Kepler-93b
Comparison Kepler-93b & Earth.jpg
An artist's impression comparing the size and internal structure of Earth (left) and Kepler-93b (right).
Discovery [1]
Discovered by Geoffrey W. Marcy et al.
Discovery dateFebruary 2014 (announced)
Transit method
Designations
KIC 3544595 b, KOI-69.01, BD+38 3583b, TYC 3134-218-1 b [2]
Orbital characteristics [3]
0.05343±0.00065  AU
Eccentricity 0
4.72673978(97)  d
Inclination 89.183°±0.044°
Semi-amplitude 1.89±0.21  m/s
StarKepler-93
Physical characteristics [3]
1.478±0.019  R🜨
Mass 4.66±0.53  M🜨
Mean density
7.93+0.96
−0.94  g/cm3
Temperature 1133±17  K (860 °C; 1,580 °F, equilibrium)

    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]

    Contents

    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] In 2023, the planet's mass was revised upward to 4.66±0.53ME, placing its density at 7.93+0.96
    −0.94     g/cm3, [3] roughly the same as the metal iron (7.874  g/cm3 ). [10]

    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%), [11] compared to the 32.5 ± 0.1% of Earth and 31 ± 1% of Venus. [11]

    The planet orbits its host star every 4.73 days [8] at a distance of 0.05343 AU (7,993,000 km), [3] 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. [lower-alpha 1]

    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, [14] has a temperature of 5,772 K (5,499 °C; 9,930 °F) and a spectral type of G2V. [15] The apparent magnitude of the star is 9.931, [9] making it too dim to be visible from Earth by the naked eye. [16]

    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

    Footnotes

    1. ↑ The temperature of lava is typically at 800–1,200 °C (1,070–1,470 K; 1,470–2,190 °F); [12] aluminium melts at 660.32 °C (933.47 K; 1,220.58 °F). [13]

    Related Research Articles

    <span class="mw-page-title-main">Super-Earth</span> Type of exoplanet

    A Super-Earth is a type of exoplanet with a mass higher than Earth's, but substantially below those of the Solar System's ice giants, Uranus and Neptune, which are 14.5 and 17 times Earth's, respectively. The term "super-Earth" refers only to the mass of the planet, and so does not imply anything about the surface conditions or habitability. The alternative term "gas dwarfs" may be more accurate for those at the higher end of the mass scale, although "mini-Neptunes" is a more common term.

    <span class="mw-page-title-main">Kepler-4b</span> Extrasolar planet in the constellation Draco

    Kepler-4b, initially known as KOI 7.01, is an extrasolar planet first detected as a transit by the Kepler spacecraft. Its radius and mass are similar to that of Neptune; however, due to its proximity to its host star, it is substantially hotter than any planet in the Solar System. The planet's discovery was announced on January 4, 2010, in Washington, D.C., along with four other planets that were initially detected by the Kepler spacecraft and subsequently confirmed by telescopes at the W.M. Keck Observatory.

    <span class="mw-page-title-main">Kepler-10</span> Sunlike star in the constellation Draco

    Kepler-10, formerly known as KOI-72, is a Sun-like star in the constellation of Draco that lies 607 light-years from Earth. Kepler-10 was targeted by NASA's Kepler spacecraft, as it was seen as the first star identified by the Kepler mission that could be a possible host to a small, transiting exoplanet. The star is slightly less massive, slightly larger, and slightly cooler than the Sun; at an estimated 11.9 billion years in age, Kepler-10 is 2.3 times the age of the Sun.

    <span class="mw-page-title-main">Kepler-42</span> Red dwarf star in the constellation Cygnus

    Kepler-42, formerly known as KOI-961, is a red dwarf located in the constellation Cygnus and approximately 131 light years from the Sun. It has three known extrasolar planets, all of which are smaller than Earth in radius, and likely also in mass.

    <span class="mw-page-title-main">Mini-Neptune</span> Planet smaller than Neptune with a gas atmosphere

    A Mini-Neptune is a planet less massive than Neptune but resembling Neptune in that it has a thick hydrogen-helium atmosphere, probably with deep layers of ice, rock or liquid oceans.

    Kepler-80, also known as KOI-500, is a red dwarf star of the spectral type M0V. This stellar classification places Kepler-80 among the very common, cool, class M stars that are still within their main evolutionary stage, known as the main sequence. Kepler-80, like other red dwarf stars, is smaller than the Sun, and it has both radius, mass, temperatures, and luminosity lower than that of our own star. Kepler-80 is found approximately 1,223 light years from the Solar System, in the stellar constellation Cygnus, also known as the Swan.

    Kepler-68b is an exoplanet orbiting the Sun-like star Kepler-68 in the constellation of Cygnus. Discovered by planetary-transit methods by the Kepler space telescope in February 2013, it has a radius of 2.31 ± 0.07 that of Earth and a density of 2.46–4.3 g/cm3. It has an orbital period of 5.398763 days at a distance of about 0.0617 AU from its star. Doppler measurements were made to determine its mass to be 5.79 times that of Earth.

    Kepler-32 is an M-type main sequence star located about 1053 light years from Earth, in the constellation of Cygnus. Discovered in January 2012 by the Kepler spacecraft, it shows a 0.58 ± 0.05 solar mass (M☉), a 0.53 ± 0.04 solar radius (R☉), and temperature of 3900.0 K, making it half the mass and radius of the Sun, two-thirds its temperature and 5% its luminosity.

    <span class="mw-page-title-main">Kepler-56</span> Red giant star in the constellation Cygnus

    Kepler-56 is a red giant in constellation Cygnus roughly 3,030 light-years (930 pc) away with slightly more mass than the Sun.

    <span class="mw-page-title-main">Kepler-90</span> Star in the constellation Draco, orbited by eight planets

    Kepler-90, also designated 2MASS J18574403+4918185, is a F-type star located about 2,790 light-years (855 pc) from Earth in the constellation of Draco. It is notable for possessing a planetary system that has the same number of observed planets as the Solar System.

    <span class="mw-page-title-main">Kepler-23</span> Star in the constellation Cygnus

    Kepler-23 is a G-type main-sequence star about 2,860 light-years away in the northern constellation of Cygnus, the swan. With an apparent visual magnitude of 13.5, it is too faint to be seen with the naked eye. This star is similar in mass and temperature to the Sun, but is larger and more luminous. Kepler-23 is orbited by three known exoplanets.

    <span class="mw-page-title-main">Kepler-90g</span> Super-puff exoplanet in the constellation Draco

    Kepler-90g is a super-puff exoplanet orbiting the early G-type main sequence star Kepler-90, one of eight planets around this star discovered using NASA's Kepler space telescope. It is located about 2,840 light-years (870 pc) from Earth, in the constellation Draco. The exoplanet was found by using the transit method, in which the dimming effect that a planet causes as it crosses in front of its star is measured. It orbits its parent star about every 210.5 days at a distance of 0.71 astronomical units.

    <span class="mw-page-title-main">Kepler-138</span> Red dwarf in the constellation Lyra

    Kepler-138, also known as KOI-314, is a red dwarf located in the constellation Lyra, 219 light years from Earth. It is located within the field of vision of the Kepler spacecraft, the satellite that NASA's Kepler Mission used to detect planets transiting their stars.

    Kepler-29 is a Sun-like star in the northern constellation of Cygnus. It is located at the celestial coordinates: Right Ascension 19h 53m 23.6018s, Declination +47° 29′ 28.437″. With an apparent visual magnitude of 15.456, this star is too faint to be seen with the naked eye. It is a solar analog, having a close mass, radius, and temperature as the Sun. Currently the age of the star has not been determined due to its 2780 light-year distance. As of 2016 no Jovian exoplanets of 0.9–1.4 MJ have been found at a distance of 5 AU.

    <span class="mw-page-title-main">KOI-256</span> Double star in the constellation Cygnus

    KOI-256 is a double star located in the constellation Cygnus approximately 575 light-years (176 pc) from Earth. While observations by the Kepler spacecraft suggested the system contained a gas giant exoplanet orbiting a red dwarf, later studies determined that KOI-256 was a binary system composed of the red dwarf orbiting a white dwarf.

    Kepler-89e, also known as KOI-94e, is an exoplanet in the constellation of Cygnus. It orbits Kepler-89.

    Kepler-1229 is a red dwarf star located about 875 light-years (268 pc) away from the Earth in the constellation of Cygnus. It is known to host a super-Earth exoplanet within its habitable zone, Kepler-1229b, which was discovered in 2016.

    <span class="mw-page-title-main">HD 179070</span> Star in the constellation Lyra

    HD 179070, also known as Kepler-21, is a star with a closely orbiting exoplanet in the northern constellation of Lyra. At an apparent visual magnitude of 8.25 this was the brightest star observed by the Kepler spacecraft to host a validated planet until the discovery of an exoplanet orbiting HD 212657 in 2018. This system is located at a distance of 354 light-years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −18.2 km/s.

    <span class="mw-page-title-main">Kepler-1638</span> G-type star in the constellation Cygnus

    Kepler-1638 is a G-type main-sequence star located about 5,000 light years away in the constellation of Cygnus. One known exoplanet has been found orbiting the star: Kepler-1638b.As of January 2021, Kepler-1638 is the farthest star with a known exoplanet orbiting in the habitable zone.

    Kepler-167 is a K-type main-sequence star located about 1,119 light-years (343 pc) away from the Solar System in the constellation of Cygnus. The star has about 78% the mass and 75% the radius of the Sun, and a temperature of 4,884 K. It hosts a system of four known exoplanets. There is also a companion red dwarf star at a separation of about 700 AU, with an estimated orbital period of over 15,000 years.

    References

    1. 1 2 3 4 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.
    2. ↑ "The Extrasolar Planet Encyclopaedia — Kepler-93b". Extrasolar Planets Encyclopaedia . Retrieved 2024-05-04.
    3. 1 2 3 4 5 6 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.
    4. ↑ 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.
    5. 1 2 3 "BD+38 3853". SIMBAD . Retrieved 2024-05-08.
    6. ↑ "SKY-MAP.ORG - Interactive Sky Map". Sky-Map.org . Retrieved 2024-05-08.
    7. 1 2 "Gauging an Alien World's Size". NASA. 2014-07-22. Retrieved 2024-05-07.
    8. 1 2 3 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.
    9. 1 2 3 4 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.
    10. ↑ Arblaster, John W. (2018). Selected Values of the Crystallographic Properties of Elements. Materials Park, Ohio: ASM International. ISBN   978-1-62708-155-9.
    11. 1 2 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.
    12. ↑ 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.
    13. ↑ "Technical data for the element Aluminum in the Periodic Table". The Photographic Periodic Table of the Elements. Retrieved 2024-05-31.
    14. ↑ 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)
    15. ↑ 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.
    16. ↑ John E. Bortle (February 2001). "The Bortle Dark-Sky Scale". Sky & Telescope. Archived from the original on 2009-03-23. Retrieved 2009-11-18.
    This page is based on this Wikipedia article
    Text is available under the CC BY-SA 4.0 license; additional terms may apply.
    Images, videos and audio are available under their respective licenses.