Get Alpha Centauri essential facts below. View Videos or join the Alpha Centauri discussion. Add Alpha Centauri to your PopFlock.com topic list for future reference or share this resource on social media.
Alpha Centauri A has 1.1 times the mass and 1.519 times the luminosity of the Sun, while Alpha Centauri B is smaller and cooler, at 0.907 times the Sun's mass and 0.445 times its luminosity. The pair orbit around a common centre with an orbital period of 79.91 years. Their elliptical orbit is eccentric, so that the distance between A and B varies from 35.6 AU (astronomical units), or about the distance between Pluto and the Sun, to 11.2 AU, or about the distance between Saturn and the Sun.
Alpha Centauri C, or Proxima Centauri, is a small and faint red dwarf (Class M). Though not visible to the naked eye, Proxima Centauri is the closest star to the Sun at a distance of 4.24 light-years (1.30 pc), slightly closer than Alpha Centauri AB. Currently, the distance between Proxima Centauri and Alpha Centauri AB is about 13,000 astronomical units (0.21 ly), equivalent to about 430 times the radius of Neptune's orbit. Proxima Centauri b is an Earth-sizedexoplanet in the habitable zone of Proxima Centauri; it was discovered in 2016.
? Centauri (Latinised to Alpha Centauri) is the system's designation given by Johann Bayer in 1603. It bears the traditional name Rigil Kentaurus, which is a Latinisation of the Arabic name ar-Rijl al-Qanris, meaning 'the Foot of the Centaur'.
The name is frequently abbreviated to Rigil Kent or even Rigil, though the latter name is better known for Beta Orionis (Rigel).
An alternative name found in European sources, Toliman, is an approximation of the Arabic a?-?al?m?n (in older transcription, a?-?hal?m?n), meaning 'the (two male) Ostriches', an appellation Kazwini had applied to Lambda and Mu Sagittarii, also in the southern hemisphere.
A third name that has been applied is Bungula , of obscure origin. Allen can only surmise it may have been coined from ? and Latin ungula 'hoof'.
Alpha Centauri C was discovered in 1915 by Robert T. A. Innes, who suggested that it be named Proxima Centaurus, from Latin, meaning 'the nearest [star] of Centaurus'. The name Proxima Centauri later became more widely used and is now listed by the IAU as the approved proper name.
Alpha Centauri is a triple star system, with its two main stars, Alpha Centauri A and Alpha Centauri B, being a binary component. The AB designation, or older A×B, denotes the mass centre of a main binary system relative to companion star(s) in a multiple star system.AB-C refers to the component of Proxima Centauri in relation to the central binary, being the distance between the centre of mass and the outlying companion. Because the distance between Proxima (C) and either of Alpha Centauri A or B is similar, the AB binary system is sometimes treated as a single gravitational object.
Apparent and true orbits of Alpha Centauri. The A component is held stationary, and the relative orbital motion of the B component is shown. The apparent orbit (thin ellipse) is the shape of the orbit as seen by an observer on Earth. The true orbit is the shape of the orbit viewed perpendicular to the plane of the orbital motion. According to the radial velocity vs. time, the radial separation of A and B along the line of sight had reached a maximum in 2007, with B being further from Earth than A. The orbit is divided here into 80 points: each step refers to a timestep of approx. 0.99888 years or 364.84 days.
The A and B components of Alpha Centauri have an orbital period of 79.91 years. Their orbit is moderately eccentric, e = 0.5179; their closest approach or periastron is 11.2 AU (1.68 billion km), or about the distance between the Sun and Saturn; and their furthest separation or apastron is 35.6 AU (5.33 billion km), about the distance between the Sun and Pluto. The most recent periastron was in August 1955 and the next will occur in May 2035; the most recent apastron was in May 1995 and will next occur in 2075.
Viewed from Earth, the apparent orbit of A and B means that their separation and position angle (PA) are in continuous change throughout their projected orbit. Observed stellar positions in 2019 are separated by 4.92 arcsec through the PA of 337.1°, increasing to 5.49 arcsec through 345.3° in 2020. The closest recent approach was in February 2016, at 4.0 arcsec through the PA of 300°. The observed maximum separation of these stars is about 22 arcsec, while the minimum distance is 1.7 arcsec. The widest separation occurred during February 1976, and the next will be in January 2056.
Alpha Centauri C is about 13,000 AU away from Alpha Centauri AB. This is equivalent to 0.21 ly or 1.9 trillion km--about 5% the distance between Alpha Centauri AB and the Sun. Until 2017, measurements of its small speed and its trajectory were of too little accuracy and duration in years to determine whether it is bound to Alpha Centauri AB or unrelated.
Radial velocity measurements made in 2017 were precise enough to show that Proxima Centauri and Alpha Centauri AB are gravitationally bound. The orbital period of Proxima Centauri is approximately years, with an eccentricity of 0.50 ± 0.08, much more eccentric than Mercury's. Proxima Centauri comes within of AB at periastron, and its apastron occurs at .
The relative sizes and colours of stars in the Alpha Centauri system, compared to the Sun
Asteroseismic studies, chromospheric activity, and stellar rotation (gyrochronology) are all consistent with the Alpha Centauri system being similar in age to, or slightly older than, the Sun. Asteroseismic analyses that incorporate tight observational constraints on the stellar parameters for the Alpha Centauri stars have yielded age estimates of Gyr, Gyr, 5.2 ± 1.9 Gyr, 6.4 Gyr, and Gyr. Age estimates for the stars based on chromospheric activity (Calcium H & K emission) yield 4.4 ± 2.1 Gyr, whereas gyrochronology yields Gyr.Stellar evolution theory implies both stars are slightly older than the Sun at 5 to 6 billion years, as derived by their mass and spectral characteristics.
From the orbital elements, the total mass of Alpha Centauri AB is about 2.0 M☉[note 2]--or twice that of the Sun. The average individual stellar masses are 1.09 M☉ and 0.90 M☉, respectively, though slightly higher masses have been quoted in recent years, such as 1.14 M☉ and 0.92 M☉, or totalling 2.06 M☉. Alpha Centauri A and B have absolute magnitudes of +4.38 and +5.71, respectively.
Alpha Centauri A
Alpha Centauri A, also known as Rigil Kentaurus, is the principal member, or primary, of the binary system. It is a solar-like main-sequence star with a similar yellowish colour, whose stellar classification is spectral type G2 V; it is slightly larger and more luminous than the Sun. Alpha Centauri A is about 10 percent more massive than the Sun, with a radius about 22 percent larger. When considered among the individual brightest stars in the sky (excluding the Sun), it is the fourth brightest at an apparent magnitude of -0.01, being slightly fainter than Arcturus at an apparent magnitude of -0.04.
The type of magnetic activity on Alpha Centauri A is comparable to that of the Sun, showing coronal variability due to star spots, as modulated by the rotation of the star. However, since 2005 the activity level has fallen into a deep minimum that might be similar to the Sun's historical Maunder Minimum. Alternatively, it may have a very long stellar activity cycle and is slowly recovering from a minimum phase.
Alpha Centauri B
Alpha Centauri B, also known as Toliman, is the secondary star of the binary system. It is a main-sequence star of spectral type K1 V, making it more an orange colour than Alpha Centauri A; it has around 90 percent the mass of the Sun and a 14 percent smaller diameter. Although it has a lower luminosity than A, Alpha Centauri B emits more energy in the X-ray band. Its light curve varies on a short time scale, and there has been at least one observed flare. It is more magnetically active than Alpha Centauri A, showing a cycle of compared to 11 years for the Sun, and about half the minimum-to-peak variation in coronal luminosity of the Sun. Alpha Centauri B has an apparent magnitude of +1.35, slightly dimmer than Mimosa.
Alpha Centauri C (Proxima Centauri)
Alpha Centauri C, better known as Proxima Centauri, is a small main-sequence red dwarf of spectral class M6 Ve. It has an absolute magnitude of +15.60, over 20,000 times fainter than the Sun. Its mass is calculated to be M☉.
Relative positions of Sun, Alpha Centauri AB and Proxima Centauri. Grey dot is projection of Proxima Centauri, located at the same distance as Alpha Centauri AB.
As seen from Earth, Proxima Centauri is 2.2° southwest from Alpha Centauri AB, about four times the angular diameter of the Moon. Proxima Centauri appears as a deep-red star of a typical apparent magnitude of 11.1 in a sparsely populated star field, requiring moderately sized telescopes to be seen. Listed as V645 Cen in the General Catalogue of Variable Stars Version 4.2, this UV Ceti-type flare star can unexpectedly brighten rapidly by as much as 0.6 magnitudes at visual wavelengths, then fade after only a few minutes. Some amateur and professional astronomers regularly monitor for outbursts using either optical or radio telescopes. In August 2015, the largest recorded flares of the star occurred, with the star becoming 8.3 times brighter than normal on 13 August, in the B band (blue light region).
Alpha Centauri is listed in the 2nd-century star catalog of Ptolemy. He gave its ecliptic coordinates, but texts differ as to whether the ecliptic latitude reads or . (Presently the ecliptic latitude is , but it has decreased by a fraction of a degree since Ptolemy's time due to proper motion.) In Ptolemy's time, Alpha Centauri was visible from Alexandria, Egypt, at but, due to precession, its declination is now , and it can no longer be seen at that latitude. English explorer Robert Hues brought Alpha Centauri to the attention of European observers in his 1592 work Tractatus de Globis, along with Canopus and Achernar, noting:
Now, therefore, there are but three Stars of the first magnitude that I could perceive in all those parts which are never seene here in England. The first of these is that bright Star in the sterne of Argo which they call Canobus. The second [Achernar] is in the end of Eridanus. The third [Alpha Centauri] is in the right foote of the Centaure.
The binary nature of Alpha Centauri AB was recognised in December 1689 by Jean Richaud, while observing a passing comet from his station in Puducherry. Alpha Centauri was only the second binary star to be discovered, preceded by Acrux.
The large proper motion of Alpha Centauri AB was discovered by Manuel John Johnson, observing from Saint Helena, who informed Thomas Henderson at the Royal Observatory, Cape of Good Hope of it. The parallax of Alpha Centauri was subsequently determined by Henderson from many exacting positional observations of the AB system between April 1832 and May 1833. He withheld his results, however, because he suspected they were too large to be true, but eventually published them in 1839 after Friedrich Wilhelm Bessel released his own accurately determined parallax for 61 Cygni in 1838. For this reason, Alpha Centauri is sometimes considered as the second star to have its distance measured because Henderson's work was not fully acknowledged at first. (The distance of Alpha Centauri from the Earth is now reckoned at 4.396 ly or 41.59 trillion km.)
Compared to the Sun, Alpha Centauri A is of the same stellar type G2, while Alpha Centauri B is a K1-type star.
By 1926, William Stephen Finsen calculated the approximate orbit elements close to those now accepted for this system. All future positions are now sufficiently accurate for visual observers to determine the relative places of the stars from a binary star ephemeris. Others, like D. Pourbaix (2002), have regularly refined the precision of new published orbital elements.
Robert T. A. Innes discovered Proxima Centauri in 1915 by blinking photographic plates taken at different times during a proper motion survey. These showed large proper motion and parallax similar in both size and direction to those of Alpha Centauri AB, suggesting that Proxima Centauri is part of the Alpha Centauri system and slightly closer to Earth than Alpha Centauri AB. Lying 4.24 ly (1.30 pc) away, Proxima Centauri is the nearest star to the Sun.
Stars closest to the Sun, including Alpha Centauri (25 April 2014)
All components of Alpha Centauri display significant proper motion against the background sky. Over centuries, this causes their apparent positions to slowly change. Proper motion was unknown to ancient astronomers. Most assumed that the stars are permanently fixed on the celestial sphere, as stated in the works of the philosopher Aristotle. In 1718, Edmond Halley found that some stars had significantly moved from their ancient astrometric positions.
In the 1830s, Thomas Henderson discovered the true distance to Alpha Centauri by analysing his many astrometric mural circle observations. He then realised this system also likely had a high proper motion. In this case, the apparent stellar motion was found using Nicolas Louis de Lacaille's astrometric observations of 1751-1752, by the observed differences between the two measured positions in different epochs.
Calculated proper motion of the centre of mass for Alpha Centauri AB is about 3620 mas (milli-arcseconds) per year toward the west and 694 mas/y toward the north, giving an overall motion of 3686 mas/y in a direction 11° north of west.[note 4] The motion of the centre of mass is about 6.1 arcmin each century, or 1.02° each millennium. The velocity in the western direction is 23.0 km/s and in the northerly direction 4.4 km/s. Using spectroscopy the mean radial velocity has been determined to be around 22.4 km/s towards the Solar System.
Since Alpha Centauri AB is almost exactly in the plane of the Milky Way as viewed from Earth, there are many stars behind them. In early May 2028, Alpha Centauri A will pass between us and a distant red star, when there will be a 45% probability that an Einstein ring will be observed. Other conjunctions will also occur in the coming decades, allowing accurate measurement of proper motions and possibly giving information on planets.
Predicted future changes
Distances of the nearest stars from 20,000 years ago until 80,000 years in the future
Animation showing motion of Alpha Centauri through the sky. (The other stars are held fixed for didactic reasons.) "Oggi" means today.
Based on the system's common known proper motion and radial velocities, Alpha Centauri will continue to change its position in the sky significantly and will gradually brighten. For example, in about 6,200 AD, ? Centauri's true motion will cause an extremely rare first-magnitude stellar conjunction with Beta Centauri, forming a brilliant optical double star in the southern sky. It will then pass just north of the Southern Cross or Crux, before moving northwest and up towards the present celestial equator and away from the galactic plane. By about 26,700 AD, in the present-day constellation of Hydra, Alpha Centauri will reach perihelion at 0.90 pc or 2.9 ly away, though later calculations suggest that this will occur in 27,000 AD. At nearest approach, Alpha Centauri will attain a maximum apparent magnitude of -0.86, comparable to present-day magnitude of Canopus, but it will still not surpass that of Sirius, which will brighten incrementally over the next 60,000 years, and will continue to be the brightest star as seen from Earth (other than the Sun) for the next 210,000 years.
Only one planet has been confirmed for the Alpha Centauri system: Proxima Centauri b. It is slightly larger than the Earth, and orbits around Proxima Centauri in its habitable zone. The existence of Proxima Centauri b was announced in 2016 by the European Southern Observatory. It was found using the radial velocity method, where periodic Doppler shifts of spectral lines of the host star suggest an orbiting object.
Controversial and hypothetical planets
Alpha Centauri Bb
In 2012, a planet around Alpha Centauri B was announced, Alpha Centauri Bb, but in 2015 a new analysis concluded that it almost certainly does not exist and was just a spurious artefact of the data analysis.
Whilst ruling out the existence of Alpha Centauri Bb, a possible transit of a separate exoplanet in 2013 was observed. The transit event could correspond to a planetary body with a radius around 0.92 R?. This planet would most likely orbit Alpha Centauri B with an orbital period of 20.4 days or less, with only a 5 percent chance of it having a longer orbit. The median of the likely orbits is 12.4 days with an impact parameter of around 0-0.3. Its orbit would likely have an eccentricity of 0.24 or less. Like the probably spurious Alpha Centauri Bb, it likely has lakes of molten lava and would be far too close to Alpha Centauri B to harbour life.
Additional planets may exist in the Alpha Centauri system, either orbiting Alpha Centauri A or Alpha Centauri B individually, or in large orbits around Alpha Centauri AB. Because both stars are fairly similar to the Sun (for example, in age and metallicity), astronomers have been especially interested in making detailed searches for planets in the Alpha Centauri system. Several established planet-hunting teams have used various radial velocity or star transit methods in their searches around these two bright stars. All the observational studies have so far failed to find evidence for brown dwarfs or gas giants.
In 2009, computer simulations showed that a planet might have been able to form near the inner edge of Alpha Centauri B's habitable zone, which extends from 0.5 to 0.9 AU from the star. Certain special assumptions, such as considering that the Alpha Centauri pair may have initially formed with a wider separation and later moved closer to each other (as might be possible if they formed in a dense star cluster), would permit an accretion-friendly environment farther from the star. Bodies around Alpha Centauri A would be able to orbit at slightly farther distances due to its stronger gravity. In addition, the lack of any brown dwarfs or gas giants in close orbits around Alpha Centauri make the likelihood of terrestrial planets greater than otherwise. A theoretical study indicates that a radial velocity analysis might detect a hypothetical planet of 1.8 M? in Alpha Centauri B's habitable zone.
Current estimates place the probability of finding an Earth-like planet around Alpha Centauri at roughly 75%. The observational thresholds for planet detection in the habitable zones by the radial velocity method are currently (2017) estimated to be about 50 M? for Alpha Centauri A, 8 M? for Alpha Centauri B, and 0.5 M? for Proxima Centauri.
Early computer-generated models of planetary formation predicted the existence of terrestrial planets around both Alpha Centauri A and B,[note 5] but most recent numerical investigations have shown that the gravitational pull of the companion star renders the accretion of planets difficult. Despite these difficulties, given the similarities to the Sun in spectral types, star type, age and probable stability of the orbits, it has been suggested that this stellar system could hold one of the best possibilities for harbouring extraterrestrial life on a potential planet.
In the Solar System, Jupiter and Saturn were probably crucial in perturbing comets into the inner Solar System, providing the inner planets with a source of water and various other ices. In the Alpha Centauri system, Proxima Centauri may have influenced the planetary disk as the Alpha Centauri system was forming, enriching the area around Alpha Centauri with volatile materials. This would be discounted if, for example, Alpha Centauri B happened to have gas giants orbiting Alpha Centauri A (or vice versa), or if Alpha Centauri A and B themselves were able to perturb comets into each other's inner system as Jupiter and Saturn presumably have done in the Solar System. Such icy bodies probably also reside in Oort clouds of other planetary systems. When they are influenced gravitationally by either the gas giants or disruptions by passing nearby stars, many of these icy bodies then travel star-wards. Such ideas also apply to the close approach of Alpha Centauri or other stars to the Solar System, when, in the distant future, the Oort Cloud might be disrupted enough to increase the number of active comets.
To be in the habitable zone, a planet around Alpha Centauri A would have an orbital radius of between about 1 and so as to have similar planetary temperatures and conditions for liquid water to exist. For the slightly less luminous and cooler Alpha Centauri B, the habitable zone is between about 0.7 and .
With the goal of finding evidence of such planets, both Proxima Centauri and Alpha Centauri AB were among the listed "Tier 1" target stars for NASA'sSpace Interferometry Mission (SIM). Detecting planets as small as three Earth-masses or smaller within two AU of a "Tier 1" target would have been possible with this new instrument. The SIM mission, however, was cancelled due to financial issues in 2010.
Based on observations between 2007 and 2012, a study found a slight excess of emissions in the 24 µm (mid/far-infrared) band surrounding , which may be interpreted as evidence for a sparse circumstellar disc or dense interplanetary dust. The total mass was estimated to be between 10-7 to 10-6 the mass of the Moon, or 10-100 times the mass of the Solar System's zodiacal cloud. If such a disc existed around both stars, disc would likely be stable to 2.8 AU, and would likely be stable to 2.5 AU. This would put A's disc entirely within the frost line, and a small part of B's outer disc just outside.
In modern literature, Rigil Kent (also Rigel Kent and variants;[note 7]) and Toliman, are used as colloquial alternative names of Alpha Centauri (then became the proper name of Alpha Centauri B in 10 August 2018 by approval of IAU).
Rigil Kent is short for Rigil Kentaurus, which is sometimes further abbreviated to Rigil or Rigel, though that is ambiguous with Beta Orionis, which is also called Rigel.
The name Toliman originates with Jacobus Golius' 1669 edition of Al-Farghani's Compendium. Tolimân is Golius' latinisation of the Arabic name ? al-?ulm?n "the ostriches", the name of an asterism of which Alpha Centauri formed the main star.
During the 19th century, the northern amateur popularist Elijah H. Burritt used the now-obscure name Bungula, possibly coined from "?" and the Latinungula ("hoof").
Together, Alpha and Beta Centauri form the "Southern Pointers" or "The Pointers", as they point towards the Southern Cross, the asterism of the constellation of Crux.
In January 2017, Breakthrough Initiatives and the ESO entered a collaboration to search for habitable planets in the Alpha Centauri system. The agreement involves Breakthrough Initiatives providing funding for an upgrade to the VISIR (VLT Imager and Spectrometer for mid-Infrared) instrument on ESO's Very Large Telescope (VLT) in Chile. This upgrade will greatly increase the likelihood of planet detection in the system.
^This is calculated for a fixed latitude by knowing the star's declination (?) using the formulae (90°+ ?). Alpha Centauri's declination is -60° 50?, so the observed latitude where the star is circumpolar will be south of -29° 10'S or 29°. Similarly, the place where Alpha Centauri never rises for northern observers is north of the latitude (90°+ ?) N or +29°N.
^Proper motions are expressed in smaller angular units than arcsec, being measured in milli-arcsec (mas.) or one-thousandth of an arcsec. Negative values for proper motion in RA indicate the sky motion is from east to west, and in declination north to south.
^The coordinates of the Sun would be diametrically opposite Alpha Centauri AB, at ?= 02h 39m 36.4951s, ?=+60° 50′ 02.308″
^Spellings include Rigjl Kentaurus, Hyde T., "Ulugh Beighi Tabulae Stellarum Fixarum", Tabulae Long. ac Lat. Stellarum Fixarum ex Observatione Ulugh Beighi, Oxford, 1665, p. 142., Hyde T., "In Ulugh Beighi Tabulae Stellarum Fixarum Commentarii", op. cit., p. 67., Portuguese Riguel Kentaurus da Silva Oliveira, R., "Crux Australis: o Cruzeiro do Sul"Archived 6 December 2013 at the Wayback Machine, Artigos: Planetario Movel Inflavel AsterDomus.
^Weighted parallax based on parallaxes from van Altena et al. (1995) and Söderhjelm (1999).
^ abcdefDucati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237: 0. Bibcode:2002yCat.2237....0D.
^ abValenti, Jeff A.; Fischer, Debra A. (2005). "Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs". The Astrophysical Journal Supplement Series. 159 (1): 141-166. Bibcode:2005ApJS..159..141V. doi:10.1086/430500. ISSN0067-0049.
^Raassen, A. J. J; Ness, J.-U; Mewe, R; Van Der Meer, R. L. J; Burwitz, V; Kaastra, J. S (2003). "Chandra-LETGS X-ray observation of ? Centauri: A nearby (G2V + K1V) binary system". Astronomy & Astrophysics. 400 (2): 671-678. Bibcode:2003A&A...400..671R. doi:10.1051/0004-6361:20021899.
^? ?, in Edward William Lane, An Arabic-English Lexicon
^Innes, R. T. A. (October 1915). "A Faint Star of Large Proper Motion". Circular of the Union Observatory Johannesburg. 30: 235-236. Bibcode:1915CiUO...30..235I.
^Innes, R. T. A. (September 1917). "Parallax of the Faint Proper Motion Star Near Alpha of Centaurus. 1900. R.A. 14 h 22 m 55s.-0s 6t. Dec-62° 15'2 0'8 t". Circular of the Union Observatory Johannesburg. 40: 331-336. Bibcode:1917CiUO...40..331I.
^ ab"The Colour of Stars". Australia Telescope, Outreach and Education. Commonwealth Scientific and Industrial Research Organisation. 21 December 2004. Archived from the original on 22 February 2012. Retrieved 2012.
^Benedict, G. Fritz; et al. (1998). Donahue, R. A.; Bookbinder, J. A. (eds.). Proxima Centauri: Time-resolved Astrometry of a Flare Site using HST Fine Guidance Sensor 3. ASP Conf. Ser. 154, The Tenth Cambridge Workshop on Cool Stars, Stellar Systems and the Sun. p. 1212. Bibcode:1998ASPC..154.1212B.
^Herschel, J. F. W. (1847). Results of Astronomical Observations made during the years 1834,5,6,7,8 at the Cape of Good Hope; being the completion of a telescopic survey of the whole surface of the visible heavens, commenced in 1825. Smith, Elder and Co, London. Bibcode:1847raom.book.....H.
^N.L., de La Caillé (1976). Travels at the Cape, 1751-1753: an annotated translation of Journal historique du voyage fait au Cap de Bonne-Espérance. Translated by Raven-Hart, R. Cape Town. ISBN978-0-86961-068-8.
^Lissauer, J. J.; E. V. Quintana; J. E. Chambers; M. J. Duncan & F. C. Adams (2004). "Terrestrial Planet Formation in Binary Star Systems". Revista Mexicana de Astronomía y Astrofísica (Serie de Conferencias). 22: 99-103. arXiv:0705.3444. Bibcode:2004RMxAC..22...99L.
^Baily, Francis (1843). "The Catalogues of Ptolemy, Ulugh Beigh, Tycho Brahe, Halley, Hevelius, Deduced from the Best Authorities. With Various Notes and Corrections, and a Preface to Each Catalogue. To Which is Added the Synonym of each Star, in the Catalogues or Flamsteed of Lacaille, as far as the same can be ascertained". Memoirs of the Royal Astronomical Society. 13: 1. Bibcode:1843MmRAS..13....1B.
^Kunitzsch, P. (1976). "Naturwissenschaft und Philologie: Die arabischen Elemente in der Nomenklatur und Terminologie der Himmelskunde". Die Sterne. 52: 218. Bibcode:1976Stern..52..218K.
^Hermelink, H.; Kunitzsch, Paul (1961). "Reviewed work: Arabische Sternnamen in Europa, Paul Kunitzsch". Journal of the American Oriental Society. 81 (3): 309-312. doi:10.2307/595661. JSTOR595661.
^(in Chinese) [ AEEA (Activities of Exhibition and Education in Astronomy) ? 2006 ? 6 ? 27 ?]
^ abHamacher, Duane W.; Frew, David J. (2010). "An Aboriginal Australian Record of the Great Eruption of Eta Carinae". Journal of Astronomical History & Heritage. 13 (3): 220-234. arXiv:1010.4610. Bibcode:2010JAHH...13..220H.
^Stanbridge, W. M. (1857). "On the Astronomy and Mythology of the Aboriginies of Victoria". Transactions Philosophical Institute Victoria. 2: 137-140.
^Henderson, T. (1842). "The Parallax of ? Centauri, deduced from Mr. Maclear's Observations at the Cape of Good Hope, in the Years 1839 and 1840". Memoirs of the Royal Astronomical Society. 12: 370-371. Bibcode:1842MmRAS..12..329H.
^Maclear, T. (1851). "Determination of the Parallax of ? 1 and ?2 Centauri, from Observations made at the Royal Observatory, Cape of Good Hope, in the Years 1842-3-4 and 1848". Memoirs of the Royal Astronomical Society. 20: 98. Bibcode:1851MmRAS..20...70M.