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This is a list of confirmed exoplanets with Bayer designations.
Star | Exoplanet | Mass (MJ) | Semimajor axis (AU) | Orbital period | Discovered | Discovery method | Reference |
---|---|---|---|---|---|---|---|
α Arietis | b | 1.8±0.2 | 1.2 | 380.8±0.3 d | 2011 | Radial velocity | [1] |
α Tauri | b | 5.8±0.7 | 1.46±0.27 | 628.96±0.9 d | 2015 | Radial velocity | [2] |
β Cancri | b | 7.8±0.8 | 1.7±0.1 | 605.2±4 d | 2014 | Radial velocity | [3] |
β Pictoris | b | 11.729+1.175 −2.135 | 10.018+0.082 −0.076 | 23.593+0.248 −0.209 d | 2008 | Infrared | [4] |
β Pictoris | c | 10.139+1.175 −1.031 | 2.680+0.016 −0.015 | 3.266+0.015 −0.012 d | 2020 | Direct imaging | [5] |
β Ursae Minoris | b | 6.1±1.0 | 1.4±0.1 | 522.3±2.7 d | 2014 | Radial velocity | [6] |
γ Cephei A | b | 9.4+0.7 −1.1 | 2.05±0.06 | 903.3±1.5 d | 2002 | Doppler spectroscopy | [7] |
γ1 Leonis | b | ? | 1.19 | 429 d | 2009 | Radial velocity | [8] |
γ Librae | b | 1.02 | 1.24 | 415.2 d | 2018 | Radial velocity | [9] |
γ Librae | c | 4.58 | 2.17 | 964.6±3.1 d | 2018 | Radial velocity | [10] |
γ Piscium | b | 1.34+0.02 −0.31 | 1.32+0.05 −0.08 | 555.1+6.0 −2.5 d | 2021 | Radial velocity | [11] |
ε Coronae Borealis | b | 6.7±0.3 | 1.3 | 417.9±0.5 d | 2012 | Radial velocity | [12] |
ε Eridani | b | 0.63+0.12 −0.04 | 3.52±0.04 | 2775±5 d | 2000 | Doppler spectroscopy | [13] |
ε Indi A | b | 3.0±0.1 | 8.8+0.2 −0.1 | 10932+266 −228 d | 2018 | Radial velocity | [14] |
ε Tauri | b | 7.6±0.2 | 1.93±0.03 | 645.5±5.3 d | 2007 | Doppler spectroscopy | [15] |
ι Draconis | b | 16.4+9.3 −4 | 1.453±0.026 | 510.854±0.013 d | 2002 | Doppler spectroscopy | [16] |
ι Draconis | c | 17.0+13 −5.4 | 19.4+10 −7.7 | 68+60 −36 d | 2021 | Radial velocity | [17] |
κ Andromedae | b | 13+12 −2 | 57±133 | 242±900 y | 2012 | Direct imaging | [18] |
κ Coronae Borealis | b | 1.811±0.057 | 2.65±0.13 | 1285±14 | 2012 | Radial velocity | [19] |
μ Arae | b | 1.65±0.009 | 1.522±0.001 | 643.25±0.90 d | 2000 | Doppler spectroscopy | [20] |
μ Arae | c | 0.032±0.002 | 0.09094±0.000005 | 9.6386±0.0015 d | 2004 | Radial velocity | [21] |
μ Arae | d | 0.448±0.011 | 0.9210±0.0015 | 1310.55±0.83 d | 2006 | Doppler spectroscopy | [22] |
μ Arae | e | 5.235 | 4205.8±758.9 d | 2002 | Radial velocity | [23] | |
μ Leonis | b | 2.4±0.4 | 1.1±0.1 | 357.8±1.2 d | 2014 | Radial velocity | [24] |
μ2 Scorpii | b | 14.4±0.8 | 242.4+114.5 −52.1 | ? | 2022 | Direct imaging | [25] |
ν Octantis A | b | 2.1059 | 1.276 | 414.8 d | 2021 | Radial velocity | [26] |
ν Ophiuchi | b | 81.7±22.2 | 1.803 | 530.73±0.10 d | 2012 | Radial velocity | [27] |
ν Ophiuchi | c | 92±24.7 | 6.022 | 3188.95±6.26 d | 2012 | Radial velocity | [28] |
ξ Aquilae | b | 2.8 | 0.68 | 136.75±0.25 | 2008 | Radial velocity | [29] |
ο Coronae Borealis | b | 1.5 | 0.83 | 187.83±0.54 d | 2012 | Radial velocity | [30] |
ο Ursae Majoris | b | 4.1 | 3.9 | 1630±35 d | 2012 | Radial velocity | [31] |
π Mensae | b | 12.325+1.192 −1.384 | 3.311+0.134 −0.148 | 5.719±0.001 y | 2001 | Doppler spectroscopy | [32] |
π Mensae | c | 3.63±0.38 | 0.06839±0.0005 | 6.267852±0.000016 d | 2014 | Transit | [33] |
π Mensae | d | 3.63±0.38 | ? | 124.64+0.48 −0.52 d | 2023 | Radial velocity | [34] |
ρ1 Cancri | b | 0.824±0.007 | 0.115±0.0000011 | 14.65162±0.0007 d | 1996 | Radial velocity | [35] |
ρ1 Cancri | c | 51.2±1.3 | 0.240±0.00005 | 44.3446±0.007 d | 2002 | Radial velocity | [36] |
ρ1 Cancri | d | 3.12±0.1 | 5.77±0.11 | 5218±230 d | 2002 | Radial velocity | [37] |
ρ1 Cancri | e | 7.99+0.32 −0.33 | 0.01544±0.00005 | 17.67711 h | 2004 | Radial velocity | [38] |
ρ1 Cancri | f | 7.70±0.08 | 0.781±0.007 | 260±1.1 d | 2005 | Doppler spectroscopy | [39] |
ρ Coronae Borealis | b | 1.093±0.023 | 0.2245+0.0023 −0.0024 | 39.8438±0.0027 d | 1997 | Radial velocity | [40] |
ρ Coronae Borealis | c | 28.2±1.5 | 0.4206+0.0044 −0.0024 | 102.19+0.27 −0.22 d | 2016 | Radial velocity | [41] |
ρ Coronae Borealis | d | 21.6±2.5 | 0.827±0.011 | 282.2+2.2 −3.7 d | 2023 | Radial velocity | [42] |
ρ Coronae Borealis | e | 3.79+0.53 −0.54 | 0.1061±0.0011 | 12.949±0.014 d | 2023 | Radial velocity | [43] |
τ Boötis | b | 5.5±6 | 0.0481 | 3.312463±0.000014 d | 1996 | Radial velocity | [44] |
τ Ceti | e | 3.93+0.83 −0.64 | 0.538±0.006 | 162.87+1.08 −0.46 d | 2012 | Radial velocity | [45] |
τ Ceti | f | 3.93+1.05 −1.37 | 1.334+0.017 −0.044 | 636.13+11.70 −47.69 d | 2012 | Direct imaging | [46] |
τ Ceti | g | 1.75+0.25 −0.40 | 0.133+0.001 −0.002 | 20+0.02 −0.01 d | 2017 | Radial velocity | [47] |
τ Ceti | h | 1.83+0.68 −0.26 | 0.243±0.003 | 49.41+0.08 −0.10 d | 2017 | Radial velocity | [48] |
τ Geminorum | b | 20.6 | 1.17 | 305.5±0.1 d | 2004 | Radial velocity | [49] |
υ Andromedae | b | 1.7+0.33 −0.24 | 0.0594±0.0003 | 4.61711±0.000014 d | 1996 | Radial velocity | [50] |
υ Andromedae | c | 13.98+2.3 −5.3 | 0.829±0.043 | 241.26±0.64 d | 1999 | Radial velocity | [51] |
υ Andromedae | d | 10.25+0.7 −3.3 | 0.1061±0.0011 | 1.27646±0.57 d | 1999 | Radial velocity | [52] |
υ Leonis | b | 0.51+0.06 −0.26 | 1.18+0.11 −0.32 | 385.2+2.8 −1.3 d | 2021 | Radial velocity | [53] |
ψ1 Aquarii | b | 3.2 | 0.7 | 181.4±0.1 d | 2013 | Radial velocity | [54] |
ω Serpentis | b | 1.7 | 1.q | 277.02+0.52 −0.51 d | 2013 | Radial velocity | [55] |
Upsilon Andromedae is a binary star located 44 light-years from Earth in the constellation of Andromeda. The system consists of an F-type main-sequence star and a smaller red dwarf.
Mu Arae, often designated HD 160691, officially named Cervantessur-VAN-teez, is a main sequence G-type star approximately 50 light-years away from the Sun in the constellation of Ara. The star has a planetary system with four known extrasolar planets, three of them with masses comparable with that of Jupiter. Mu Arae c, the innermost, was the first hot Neptune or super-Earth discovered.
55 Cancri is a binary star system located 41 light-years away from the Sun in the zodiac constellation of Cancer. It has the Bayer designation Rho1 Cancri (ρ1 Cancri); 55 Cancri is the Flamsteed designation. The system consists of a K-type star and a smaller red dwarf.
Rho Coronae Borealis is a yellow dwarf star 57.1 light-years away in the constellation of Corona Borealis. The star is thought to be similar to the Sun with nearly the same mass, radius, and luminosity. It is orbited by four known exoplanets.
Tau Boötis b, or more precisely Tau Boötis Ab, is an extrasolar planet approximately 51 light-years away. The planet and its host star is one of the planetary systems selected by the International Astronomical Union as part of NameExoWorlds, their public process for giving proper names to exoplanets and their host star. The process involved public nomination and voting for the new names, and the IAU planned to announce the new names in mid-December 2015. However, the IAU annulled the vote as the winning name was judged not to conform with the IAU rules for naming exoplanets.
Sudarsky's classification of gas giants for the purpose of predicting their appearance based on their temperature was outlined by David Sudarsky and colleagues in the paper Albedo and Reflection Spectra of Extrasolar Giant Planets and expanded on in Theoretical Spectra and Atmospheres of Extrasolar Giant Planets, published before any successful direct or indirect observation of an extrasolar planet atmosphere was made. It is a broad classification system with the goal of bringing some order to the likely rich variety of extrasolar gas-giant atmospheres.
14 Andromedae, abbreviated 14 And, also named Veritate, is a single, orange-hued giant star situated approximately 247 light-years away in the northern constellation of Andromeda. It is dimly visible to the naked eye with an apparent visual magnitude of 5.22. The star is moving closer to the Earth with a heliocentric radial velocity of −60 km/s. In 2008 an extrasolar planet was discovered to be orbiting the star.
55 Cancri b, occasionally designated 55 Cancri Ab, also named Galileo, is an exoplanet orbiting the Sun-like star 55 Cancri A every 14.65 days. It is the second planet in order of distance from its star, and is an example of a hot Jupiter, or possibly rather "warm Jupiter".
55 Cancri c, formally named Brahe, is an extrasolar planet in an eccentric orbit around the Sun-like star 55 Cancri A, making one revolution every 44.34 days. It is the third known planet in order of distance from its star. 55 Cancri c was discovered on June 13, 2002, and has a mass roughly half of Saturn.
Upsilon Andromedae b, formally named Saffar, is an extrasolar planet approximately 44 light-years away from the Sun in the constellation of Andromeda. The planet orbits the solar analog star, Upsilon Andromedae A, approximately every five days. Discovered in June 1996 by Geoffrey Marcy and R. Paul Butler, it was one of the first hot Jupiters to be discovered. It is also one of the first non-resolved planets to be detected directly. Upsilon Andromedae b is the innermost-known planet in its planetary system.
Upsilon Andromedae c, formally named Samh, is an extrasolar planet orbiting the Sun-like star Upsilon Andromedae A every 241.3 days at an average distance of 0.83 AU. Its discovery in April 1999 by Geoffrey Marcy and R. Paul Butler made this the first multiple-planet system to be discovered around a main-sequence star, and the first multiple-planet system known in a multiple star system. Upsilon Andromedae c is the second-known planet in order of distance from its star.
HD 70642 b is an exoplanet orbiting the star HD 70642 at a distance of 3.23 AU, taking 5.66 years to complete an orbit. This planet may have systems of moons like Jupiter. This planet was discovered on July 3, 2003. It is located about 95 light-years away in the constellation Puppis. In 2023, the inclination and true mass of HD 70642 b were determined via astrometry.
55 Cancri f, also designated Rho1 Cancri f and formally named Harriot, is an exoplanet approximately 41 light-years away from Earth in the constellation of Cancer. 55 Cancri f is the fourth known planet from the star 55 Cancri and the first planet to have been given the designation of "f".
14 Andromedae b, formally named Spe, is an exoplanet approximately 249 light years away in the constellation of Andromeda.
81 Ceti b is an extrasolar planet approximately 331 light years away in the constellation of Cetus. It is estimated to be 5.3 times the mass of Jupiter which also makes it a gas giant. It orbits the G-type giant star 81 Ceti at an average distance of 2.5 AU, taking about 2.6 years to revolve with an eccentricity of 20.6.
An exoplanet is a planet located outside the Solar System. The first evidence of an exoplanet was noted as early as 1917, but was not recognized as such until 2016; no planet discovery has yet come from that evidence. What turned out to be the first detection of an exoplanet was published among a list of possible candidates in 1988, though not confirmed until 2003. The first confirmed detection came in 1992, with the discovery of terrestrial-mass planets orbiting the pulsar PSR B1257+12. The first confirmation of an exoplanet orbiting a main-sequence star was made in 1995, when a giant planet was found in a four-day orbit around the nearby star 51 Pegasi. Some exoplanets have been imaged directly by telescopes, but the vast majority have been detected through indirect methods, such as the transit method and the radial-velocity method. As of 1 September 2023, there are 5,506 confirmed exoplanets in 4,065 planetary systems, with 878 systems having more than one planet. This is a list of the most notable discoveries.
The exoplanet naming convention is an extension of the system used for naming multiple-star systems as adopted by the International Astronomical Union (IAU). For exoplanets orbiting a single star, the name is normally formed by taking the name of its parent star and adding a lowercase letter. A provisional IAU-sanctioned standard exists to accommodate the naming of planets that orbit two stars, which are known as circumbinary planets. A limited number of exoplanets have IAU-sanctioned proper names. Other naming systems exist.