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List of nearest stars - Wikipedia

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Stars and brown dwarfs within 20 light years of the Solar System

Animated 3D map of the nearest stars, centered on the Sun. 3D red green glasses are recommended to view this image correctly. A radar map of all known stellar and substellar objects within 9 light years (ly), arranged clockwise in hours of right ascension, and marked by distance (▬) and position (◆). Distances are marked outward from the Sun (Sol), with concentric circles indicating the distance in one ly steps. Positions are marked inward from their distance markings, connected by lines according to their declinations (doted when positive), representing the arcs of the declinations viewed edge-on. For within 12 ly see this map.

This list covers all known stars, white dwarfs, brown dwarfs, and sub-brown dwarfs within 20 light-years (6.13 parsecs) of the Sun. So far, 131 such objects have been found. Only 22 are bright enough to be visible without a telescope, for which the star's visible light needs to reach or exceed the dimmest brightness visible to the naked eye from Earth, which is typically around 6.5 apparent magnitude.^[1]

The known 131 objects are bound in 94 stellar systems. Of those, 103 are main sequence stars: 80 red dwarfs and 23 "typical" stars having greater mass. Additionally, astronomers have found 6 white dwarfs (stars that have exhausted all fusible hydrogen), 21 brown dwarfs, as well as 1 sub-brown dwarf, WISE 0855−0714 (possibly a rogue planet). The closest system is Alpha Centauri, with Proxima Centauri as the closest star in that system, at 4.2465 light-years from Earth. The brightest, most massive and most luminous object among those 131 is Sirius A, which is also the brightest star in Earth's night sky; its white dwarf companion Sirius B is the hottest object among them. The largest object within the 20 light-years is Procyon.

The Solar System, and the other stars/dwarfs listed here, are currently moving within (or near) the Local Interstellar Cloud, roughly 30 light-years (9.2 pc) across. The Local Interstellar Cloud is, in turn, contained inside the Local Bubble, a cavity in the interstellar medium about 300 light-years (92.0 pc) across. It contains Ursa Major and the Hyades star cluster, among others. The Local Bubble also contains the neighboring G-Cloud, which contains the stars Alpha Centauri and Altair. In the galactic context, the Local Bubble is a small part of the Orion Arm, which contains most stars that we can see without a telescope. The Orion Arm is one of the spiral arms of our Milky Way galaxy.

The easiest way to determine stellar distance to the Sun for objects at these distances is parallax, which measures how much stars appear to move against background objects over the course of Earth's orbit around the Sun. As a parsec (parallax-second) is defined by the distance of an object that would appear to move exactly one second of arc against background objects, stars less than 5 parsecs away will have measured parallaxes of over 0.2 arcseconds, or 200 milliarcseconds. Determining past and future positions relies on accurate astrometric measurements of their parallax and total proper motions (how far they move across the sky due to their actual velocity relative to the Sun), along with spectroscopically determined radial velocities (their speed directly towards or away from us, which combined with proper motion defines their true movement through the sky relative to the Sun). Both of these measurements are subject to increasing and significant errors over very long time spans, especially over the several thousand-year time spans it takes for stars to noticeably move relative to each other.^[2]

Based on results from the Gaia telescope's second data release from April 2018, an estimated 694 stars will approach the Solar System to less than 5 parsecs in the next 15 million years. Of these, 26 have a good probability to come within 1.0 parsec (3.3 light-years) and another 7 within 0.5 parsecs (1.6 light-years).^[3] This number is likely much higher, due to the sheer number of stars needed to be surveyed; a star approaching the Solar System 10 million years ago, moving at a typical Sun-relative 20–200 kilometers per second, would be 600–6,000 light-years from the Sun at present day, with millions of stars closer to the Sun. The closest encounter to the Sun so far predicted is the low-mass orange dwarf star Gliese 710 / HIP 89825 with roughly 60% the mass of the Sun.^[4] It is currently predicted to pass 0.1696±0.0065 ly (10635±500 au) from the Sun in 1.290±0.04 million years from the present, close enough to significantly disturb the Solar System's Oort cloud.^[5]

Stars within 11 ly. Stars and star systems within 12.5 ly. Hipparcos luminous stars distances map within 100 pc (330 ly). The number in square brackets is height above or below the galactic plane. The distance between stars is colour coded: < 25 pc: green < 50 pc: cyan < 75 pc: yellow < 100 pc: orange

The classes of the stars and brown dwarfs are shown in the color of their spectral types (these colors are derived from conventional names for the spectral types and do not necessarily represent the star's observed color). Many brown dwarfs are not listed by visual magnitude but are listed by near-infrared J band apparent magnitude due to how dim (and often invisible) they are in visible color bands (U, B or V). Absolute magnitude (with electromagnetic wave, 'light' band denoted in subscript) is a measurement at a 10-parsec distance across imaginary empty space devoid of all its sparse dust and gas. Some of the parallaxes and resultant distances are rough measurements.^[6]

Distant future and past encounters[edit] Distances of the nearest stars from 20,000 years ago until 80,000 years in the future Visualisation of the orbit of the Sun (yellow dot and white curve) around the Galactic Centre (GC) in the last galactic year. The red dots correspond to the positions of the stars studied by the European Southern Observatory in a monitoring programme.^[74]

Over long periods of time, the slow independent motion of stars change in both relative position and in their distance from the observer. This can cause other currently distant stars to fall within a stated range, which may be readily calculated and predicted using accurate astrometric measurements of parallax and total proper motions, along with spectroscopically determined radial velocities. Although extrapolations can be made into the past or future, they are subject to increasingly significant cumulative errors over very long periods.^[2] Inaccuracies of these measured parameters make determining the true minimum distances of any encountering stars or brown dwarfs fairly difficult.^[75]

One of the first stars known to approach the Sun particularly close is Gliese 710. The star, whose mass is roughly half that of the Sun, is currently 62 light-years from the Solar System. It was first noticed in 1999 using data from the Hipparcos satellite, and was estimated to pass less than 1.3 light-years (0.40 pc) from the Sun in 1.4 million years.^[76] With the release of Gaia's observations of the star, it has since been refined to a much closer 0.178 light-years (0.055 pc), close enough to significantly disturb objects in the Oort cloud, which extends 1.2 light-years (0.37 pc) from the Sun.^[77]

Gaia's third data release has provided updated values for many of the candidates in the table below.^[78]^[79]^[80]^[81]

Schematic view to scale of past and future close approaches of stars to the Sun (Up to 4.5 light-years)

^ ^a ^b Parallaxes given by RECONS are a weighted mean of values in the sources given, as well as measurements by the RECONS program.

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^ Hall, Shannon (28 May 2018). "Known Close Stellar Encounters Surge in Number". Sky and Telescope. Retrieved 2 June 2018.
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^ ^a ^b ^c ^d ^e ^f ^g ^h ⁱ ^j ^k ^l ^m ⁿ ^o ^p ^q ^r ^s ^t ^u ^v ^w ^x ^y ^z ^aa ^ab ^ac ^ad ^ae ^af ^ag ^ah ^ai ^aj ^ak ^al ^am ^an ^ao ^ap ^aq ^ar ^as ^at ^au ^av ^aw ^ax ^ay ^az ^ba ^bb ^bc ^bd "The One Hundred Nearest Star Systems". Research Consortium on Nearby Stars. 17 September 2007. Retrieved 6 November 2007.
^ ^a ^b From parallax.
^ ^a ^b ^c ^d ^e ^f ^g ^h ⁱ ^j ^k ^l ^m ⁿ ^o ^p ^q ^r ^s ^t ^u ^v ^w ^x ^y ^z ^aa ^ab ^ac ^ad ^ae ^af ^ag ^ah ^ai ^aj ^ak ^al ^am ^an ^ao ^ap ^aq ^ar ^as ^at ^au ^av ^aw ^ax ^ay ^az ^ba ^bb ^bc ^bd ^be ^bf ^bg ^bh ^bi ^bj ^bk ^bl ^bm ^bn ^bo ^bp ^bq ^br ^bs ^bt ^bu ^bv Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e).
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^ Basant, Ritvik; Luque, Rafael; Bean, Jacob; Seifahrt, Andreas; Brady, Madison; Zhao, Lily; Brown, Nina; Das, Tanya; Stürmer, Julian; Kasper, David; Gupta, Rohan; Stefánsson, Guđmundur. "Four Sub-Earth Planets Orbiting Barnard's Star from MAROON-X and ESPRESSO". IOPscience. American Astronomical Society. Retrieved 14 March 2025.
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^ Jeffers, S. V.; Dreizler, S.; Barnes, J. R.; Haswell, C. A.; Nelson, R. P.; Rodríguez, E.; López-González, M. J.; Morales, N.; Luque, R.; et al. (2020), "A multiple planet system of super-Earths orbiting the brightest red dwarf star GJ887", Science, 368 (6498): 1477–1481, arXiv:2006.16372, Bibcode:2020Sci...368.1477J, doi:10.1126/science.aaz0795, PMID 32587019, S2CID 220075207
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^ General Catalogue of Trigonometric Parallaxes.
^ Hipparcos Catalogue.
^ Bessel, F. W. (1839). "Bestimmung der Entfernung des 61sten Sterns des Schwans. Von Herrn Geheimen - Rath und Ritter Bessel". Astronomische Nachrichten (in German). 16 (5–6): 65–96. Bibcode:1838AN.....16...65B. doi:10.1002/asna.18390160502. (page 92) Ich bin daher der Meinung, daß nur die jährliche Parallaxe = 0"3136 als das Resultat der bisherigen Beobachtungen zu betrachten ist A parallax of 313.6 mas yields a distance of 10.4 light years
^ Kervella, Pierre; Arenou, Frédéric; et al. (2019). "Stellar and substellar companions of nearby stars from Gaia DR2". Astronomy & Astrophysics. 623: A72. arXiv:1811.08902. Bibcode:2019A&A...623A..72K. doi:10.1051/0004-6361/201834371. S2CID 119491061. This PMa offset between 61 Cyg A and B points at the possible presence of a third body in the system, likely orbiting around 61 Cyg B.
^ Pinamonti, M.; Damasso, M.; Marzari, F.; Sozzetti, A.; Desidera, S.; Maldonado, J.; Scandariato, G.; Affer, L.; Lanza, A. F.; Bignamini, A.; Bonomo, A. S.; Borsa, F.; Claudi, R.; Cosentino, R.; Giacobbe, P.; González-Álvarez, E.; González Hernández, J. I.; Gratton, R.; Leto, G.; Malavolta, L.; Martinez Fiorenzano, A.; Micela, G.; Molinari, E.; Pagano, I.; Pedani, M.; Perger, M.; Piotto, G.; Rebolo, R.; Ribas, I.; et al. (2018). "The HADES RV Programme with HARPS-N at TNG. VIII. GJ15A: A multiple wide planetary system sculpted by binary interaction". Astronomy and Astrophysics. 617: A104. arXiv:1804.03476. Bibcode:2018A&A...617A.104P. doi:10.1051/0004-6361/201732535. S2CID 54990041.
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^ Astudillo-Defru, Nicola; Díaz, Rodrigo F.; Bonfils, Xavier; Almenara, José M.; Delisle, Jean-Baptiste; Bouchy, François; Delfosse, Xavier; Forveille, Thierry; Lovis, Christophe; Mayor, Michel; Murgas, Felipe; Pepe, Francesco; Santos, Nuno C.; Ségransan, Damien; Udry, Stéphane; Wünsche, Anaël (2017). "The HARPS search for southern extra-solar planets. XLII. A system of Earth-mass planets around the nearby M dwarf YZ Ceti". Astronomy & Astrophysics. 605: L11. arXiv:1708.03336. Bibcode:2017A&A...605L..11A. doi:10.1051/0004-6361/201731581. S2CID 119393757.
^ Astudillo-Defru, Nicola; Forveille, Thierry; Bonfils, Xavier; Ségransan, Damien; Bouchy, François; Delfosse, Xavier; et al. (2017). "The HARPS search for southern extra-solar planets. XLI. A dozen planets around the M dwarfs GJ 3138, GJ 3323, GJ 273, GJ 628, and GJ 3293". Astronomy and Astrophysics. 602. A88. arXiv:1703.05386. Bibcode:2017A&A...602A..88A. doi:10.1051/0004-6361/201630153. S2CID 119418595.
^ Pozuelos, Francisco J.; et al. (2020). "GJ 273: on the formation, dynamical evolution, and habitability of a planetary system hosted by an M dwarf at 3.75 parsec". Astronomy & Astrophysics. 641: A23. arXiv:2006.09403. Bibcode:2020A&A...641A..23P. doi:10.1051/0004-6361/202038047. S2CID 219721292.{{cite journal}}: CS1 maint: numeric names: authors list (link)
^ Caballero, J. A.; Reiners, Ansgar; Ribas, I.; Dreizler, S.; Zechmeister, M.; et al. (12 June 2019). "The CARMENES search for exoplanets around M dwarfs. Two temperate Earth-mass planet candidates around Teegarden's Star" (PDF). Astronomy & Astrophysics. 627: A49. arXiv:1906.07196. Bibcode:2019A&A...627A..49Z. doi:10.1051/0004-6361/201935460. ISSN 0004-6361. S2CID 189999121.
^ Dreizler, S.; Luque, R.; et al. (April 2024). "Teegarden's Star revisited: A nearby planetary system with at least three planets". Astronomy & Astrophysics. 684: A117. arXiv:2402.00923. Bibcode:2024A&A...684A.117D. doi:10.1051/0004-6361/202348033.
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^ Bailer-Jones, C. A. L.; Rybizki, J.; Andrae, R.; Fouesneau, M. (2010). "The discovery of a very cool, very nearby brown dwarf in the Galactic plane". Monthly Notices of the Royal Astronomical Society. 408 (1): L56. arXiv:1004.0317. Bibcode:2010MNRAS.408L..56L. doi:10.1111/j.1745-3933.2010.00927.x. S2CID 16032606.
^ Leggett, Sandy K.; Saumon, Didier; Marley, Mark S.; Lodders, Katharina; Canty, J.; Lucas, Philip W.; Smart, Richard L.; Tinney, Chris G.; Homeier, Derek; Allard, France; Burningham, Ben; Day-Jones, Avril; Fegley, Bruce; Ishii, Miki; Jones, Hugh R. A.; Marocco, Federico; Pinfield, David J.; Tamura, Motohide (2012). "The Properties of the 500 K Dwarf UGPS J072227.51-054031.2 and a Study of the Far-red Flux of Cold Brown Dwarfs". The Astrophysical Journal. 748 (2): 74. arXiv:1201.2973. Bibcode:2012ApJ...748...74L. doi:10.1088/0004-637X/748/2/74. S2CID 14171934.
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