Capella
Observation data ICRS )
| ||
---|---|---|
Constellation | Auriga | |
Pronunciation
|
/kəˈpɛlə/[1] | |
A | ||
Right ascension | 05h 16m 41.35871s[2][note 1] | |
Declination | +45° 59′ 52.7693″[2][note 1] | |
Apparent magnitude (V) | +0.08[3] (+0.03 – +0.16[4]) | |
H | ||
Right ascension | 05h 17m 23.728s[5] | |
Declination | +45° 50′ 22.97″[5] | |
Apparent magnitude (V) | 10.16[6] | |
L | ||
Right ascension | 05h 17m 23.943s[7] | |
Declination | +45° 50′ 19.84″[7] | |
Apparent magnitude (V) | 13.7[8] | |
Characteristics | ||
A | ||
Spectral type | G3III:[9] | |
U−B color index | +0.44[3] | |
B−V color index | +0.80[3] | |
V−R color index | −0.3[3] | |
R−I color index | +0.44[3] | |
Variable type | RS CVn[10] (suspected[11]) | |
Aa | ||
Evolutionary stage | Red clump[12] | |
Spectral type | K0III[13] | |
Ab | ||
Evolutionary stage | Subgiant[12] | |
Spectral type | G1III[13] | |
H | ||
Evolutionary stage | Main sequence (red dwarf)[14] | |
Spectral type | M2.5 V[15] | |
U−B color index | 1.24[16] | |
B−V color index | 1.50[14] | |
R−I color index | 0.91[14] | |
L | ||
Evolutionary stage | Main sequence (red dwarf) | |
Spectral type | M4:[17] | |
Aa | ||
Absolute magnitude (MV) | +0.296[12] | |
Ab | ||
Absolute magnitude (MV) | +0.167[12] | |
HL | ||
Radial velocity (Rv) | 31.63±0.14[12] km/s | |
H | ||
Distance | 43.38 ± 0.03 ly (13.301 ± 0.009 pc) | |
Absolute magnitude (MV) | 13.1[23] | |
Semi-amplitude (K1)(primary) | 25.9611±0.0044 km/s | |
Semi-amplitude (K2) (secondary) | 26.860±0.0017 km/s | |
Argument of periastron (ω)(secondary) | 88° | |
Details Myr | ||
Aa | ||
Rotational velocity (v sin i) | 35.0±0.5 km/s | |
H | ||
dex | ||
L | ||
Mass | 0.53[12] M☉ | |
L: 2MASS J05172394+4550198[29] | ||
Database references | ||
SIMBAD | Capella | |
Capella H | ||
Capella L |
Capella is the brightest
Although it appears to be a single star to the naked eye, Capella is actually a quadruple star system organized in two binary pairs, made up of the stars Capella Aa, Capella Ab, Capella H and Capella L. The primary pair, Capella Aa and Capella Ab, are two bright-yellow giant stars, both of which are around 2.5 times as massive as the Sun. The secondary pair, Capella H and Capella L, are around 10,000 astronomical units (AU)[note 2] from the first and are two faint, small and relatively cool red dwarfs.
Capella Aa and Capella Ab have exhausted their core
Nomenclature
α Aurigae (
The traditional name Capella is
Observational history
Capella was the brightest star in the night sky from 210,000 years ago to 160,000 years ago, at about −1.8 in apparent magnitude. At −1.1, Aldebaran was brightest before this period; it and Capella were situated rather close to each other in the sky and approximated boreal pole stars at the time.[36]
Capella is thought to be mentioned in an Akkadian inscription dating to the 20th century BC.[37] Its goat-associated symbolism dates back to Mesopotamia as a constellation called "GAM", "Gamlum" or "MUL.GAM" in the 7th-century BC document MUL.APIN. GAM represented a scimitar or crook and may have represented the star alone or the constellation of Auriga as a whole. Later, Bedouin astronomers created constellations that were groups of animals, where each star represented one animal. The stars of Auriga comprised a herd of goats, an association also present in Greek mythology.[38] It is sometimes called the Shepherd's Star in English literature.[39] Capella was seen as a portent of rain in classical times.[40]
Building J of the
Multiple status
Professor
Many observers tried to discern the component stars without success.[45] Known as "The Interferometrist's Friend", it was first resolved interferometrically in 1919 by John Anderson and Francis Pease at Mount Wilson Observatory, who published an orbit in 1920 based on their observations.[46][47] This was the first interferometric measurement of any object outside the Solar System.[48] A high-precision orbit was published in 1994 based on observations by the Mark III Stellar Interferometer, again at Mount Wilson Observatory.[49] Capella also became the first astronomical object to be imaged by a separate element optical interferometer when it was imaged by the Cambridge Optical Aperture Synthesis Telescope in September 1995.[50]
In 1914, Finnish astronomer Ragnar Furuhjelm observed that the spectroscopic binary had a faint companion star, which, as its proper motion was similar to that of the spectroscopic binary, was probably physically bound to it.[51] In February 1936, Carl L. Stearns observed that this companion appeared to be double itself;[52] this was confirmed in September that year by Gerard Kuiper. This pair are designated Capella H and L.[53]
X-ray source
Two
The X-ray luminosity (Lx) of ~1024 W (1031 erg s−1) is four orders of magnitude above the Sun's X-ray luminosity.
Observation
With an average apparent magnitude of +0.08, Capella is the brightest object in the
Capella is closer to the north
A few degrees to the southwest of Capella lie three stars, Epsilon Aurigae, Zeta Aurigae and Eta Aurigae, the latter two of which are known as "The Kids", or Haedi. The four form a familiar pattern, or asterism, in the sky.[63]
Distance
Based on an annual
In a 1960 paper, American astronomer
Stellar system
There are several stars within a few
American astronomer Robert Burnham Jr. described a scale model of the system where Capella A was represented by spheres 13 and 7 inches across, separated by ten feet. The red dwarfs were then each 0.7 inch across and they were separated by 420 feet. At this scale, the two pairs are 21 miles apart.[69]
Capella A
Capella A consists of two yellow
Modern convention designates the more luminous cooler star as component Aa and its spectral type has been usually measured between G2 and K0. The hotter secondary Ab has been given various spectral types of late (cooler) F or early (warmer) G. The
The individual apparent magnitudes of the two component stars cannot be directly measured, but their relative brightness has been measured at various wavelengths. They have very nearly equal brightness in the visible light spectrum, with the hotter secondary component generally being found to be a few tenths of a magnitude brighter.[12] A 2016 measurement gives the magnitude difference between the two stars at a wavelength of 700 nm as 0.00 ± 0.1.[72]
The physical properties of the two stars can be determined with high accuracy. The masses are derived directly from the orbital solution, with Aa being 2.5687 ± 0.0074
Estimated to be 590 to 650 million years old,
The rotational period of each star can be measured by observing periodic variations in the
Capella has long been suspected to be slightly variable. Its amplitude of about 0.1 magnitudes means that it may at times be brighter or fainter than Rigel, Betelgeuse and Vega, which are also variable. The system has been classified as an RS Canum Venaticorum variable,[10] a class of binary stars with active chromospheres that cause huge starspots, but it is still only listed as a suspected variable in the General Catalogue of Variable Stars.[11] Unusually for RS CVn systems, the hotter star, Capella Ab, has the more active atmosphere because it is located in the Hertzsprung gap—a stage where it is changing its angular momentum and deepening its convection zone.[71]
The active atmospheres and closeness of these stars means that they are among the brightest X-ray sources in the sky. However the X-ray emission is due to stable coronal structures and not eruptive flaring activity. Coronal loops larger than the Sun and with temperatures of several million kelvin are likely to be responsible for the majority of the X-rays.[74]
Capella HL
The seventh companion published for Capella, component H, is physically associated with the bright primary star. It is a
The two stars are reported to have a 3.5-visual-magnitude difference (2.3 mag in the passband of the Gaia spacecraft) although the difference is much smaller at infrared wavelengths. This is unexpected and may indicate further unseen companions.[12]
The mass of the stars can, in principle, be determined from the orbital motion, but uncertainties in the orbit have led to widely varying results. In 1975, an eccentric 388-year orbit gave masses of 0.65 M☉ and 0.13 M☉.[75] A smaller near-circular orbit published in 2015 had a 300-year orbit, benefitting from mass constraints of 0.57 M☉ and 0.53 M☉, respectively, for GJ 195 A and B, based on their infrared magnitudes.[12]
Visual companions
Six visual companions to Capella were discovered before Capella H and are generally known only as Capella B through G. None are thought to be physically associated with Capella, although all appear closer in the sky than the HL pair.[69]
Component | Primary | J2000.0 |
J2000.0 |
Epoch of observed separation |
Angular distance from primary |
Position angle (relative to primary) |
Apparent magnitude (V) |
Database reference |
---|---|---|---|---|---|---|---|---|
B | A | 05h 16m 42.7s | +46° 00′ 55″ | 1898 | 46.6 ″ |
23° | 17.1 | |
C | A | 05h 16m 35.9s | +46° 01′ 12″ | 1878 | 78.2 ″ |
318° | 15.1 | |
D | A | 05h 16m 40.1s | +45° 58′ 07″ | 1878 | 126.2 ″ |
183° | 13.6 | |
E | A | 05h 16.5m | +46° 02′ | 1908 | 154.1 ″ |
319° | 12.1 | |
F | A | 05h 16m 48.748s | +45° 58′ 30.84″ | 1999 | 112.0 ″ |
137° | 10.21 | SIMBAD |
G | A | 05h 16m 31.852s | +46° 08′ 27.42″ | 2003 | 522.4 ″ |
349° | 8.10 | SIMBAD |
Component F is also known as TYC 3358-3142-1. It is listed with a spectral type of K[76] although it is included in a catalogue of OB stars as a distant luminous star.[77]
Component G is BD+45 1076, with a spectral type of F0,
Several other stars have also been catalogued as companions to Capella.[27] Components I, Q and R are 13th-magnitude stars at distances of 92″, 133″ and 134″.[80] V538 Aurigae and its close companion HD 233153 are red dwarfs ten degrees away from Capella; they have very similar space motions but the small difference makes it possible that this is just a coincidence.[81] Two faint stars have been discovered by speckle imaging in the Capella HL field, around 10″ distant from that pair. These have been catalogued as Capella O and P. It is not known whether they are physically associated with the red dwarf binary.[82]
Etymology and culture
Capella traditionally marks the left shoulder of the constellation's eponymous charioteer, or, according to the 2nd-century astronomer Ptolemy's Almagest, the goat that the charioteer is carrying. In Bayer's 1603 work Uranometria, Capella marks the charioteer's back.[83] The three Haedi had been identified as a separate constellation by Pliny the Elder and Manilius, and were called Capra, Caper, or Hircus, all of which relate to its status as the "goat star".[40] Ptolemy merged the Charioteer and the Goats in the 2nd-century Almagest.[84]
In
In medieval accounts, it bore the uncommon name Alhajoth (also spelled Alhaior, Althaiot, Alhaiset, Alhatod, Alhojet, Alanac, Alanat, Alioc), which (especially the last) may be a corruption of its Arabic name, العيوق, al-cayyūq.
To the ancient Balts, Capella was known as Perkūno Ožka "Thunder's Goat", or Tikutis.[89] Conversely in Slavic Macedonian folklore, Capella was Jastreb "the hawk", flying high above and ready to pounce on Mother Hen (the Pleiades) and the Rooster (Nath).[90]
In
In
In Australian Aboriginal mythology for the Boorong people of Victoria, Capella was Purra, the kangaroo, pursued and killed by the nearby Gemini twins, Yurree (Castor) and Wanjel (Pollux).[100] The Wardaman people of northern Australia knew the star as Yagalal, a ceremonial fish scale, related to Guwamba the barramundi (Aldebaran).[101]
Namesakes
- Capella, a lunar crater to the north of the Mare Nectaris, not named after the star
- U.S. Navyships
- Mazda Capella, a model of automobile manufactured by Mazda
See also
- Capella in fiction
- List of brightest stars
- List of nearest bright stars
- Historical brightest stars
- List of nearest giant stars
Notes
References
- ^ "Capella". Merriam-Webster. Retrieved 2022-05-09.
- ^ S2CID 18759600.
- ^ Bibcode:1991bsc..book.....H.
- Bibcode:1990A&AS...85..971P.
- ^ ISSN 0365-0138.
- doi:10.1086/109000.
- ^ Bibcode:2003yCat.2246....0C.
- ISSN 0035-8711.
- ^ doi:10.1086/191373.
- ^ Bibcode:2002cosp...34E1599A.
- ^ Bibcode:2009yCat....102025S.
- ^ S2CID 55901109.
- ^ Bibcode:1990A&A...230..389S.
- ^ doi:10.1086/191123.; see Table 1.
- doi:10.1086/190307.
- ^ .
- ISSN 0067-0049.
- ^ .
- .
- ^ S2CID 121534198.; see Tables 3, 6 and 7.
- ^ .
- .
- doi:10.1086/161405.
- ^ doi:10.1086/171708.; see Table 1.
- ^ NAME CAPELLA – Variable of RS CVn type, database entry, SIMBAD. Accessed online December 23, 2008.
- ^ a b Brosch 2008, p. 46.
- ^ a b c "Entry 05167+4600". The Washington Double Star Catalog. United States Naval Observatory. Archived from the original on 2011-08-16. Retrieved 24 December 2008.
- ^ G 96-29 – High proper-motion Star, database entry, SIMBAD. Accessed online December 23, 2008.
- ^ NAME CAPELLA L – Star in double system, database entry, SIMBAD. Accessed online December 23, 2008.
- ISBN 978-1-931559-44-7.
- OCLC 1243068585.)
{{cite book}}
: CS1 maint: location missing publisher (link - ^ Mamajek, Eric; García, Beatriz; Hamacher, Duane; Montmerle, Thierry; Pasachoff, Jay; Ridpath, Ian; Sun, Xiaochun; van Gent, Robert (2016). "IAU Working Group on Star Names (WGSN)". Archived from the original on 10 June 2016. Retrieved 22 May 2016.
- ^ Mamajek, Eric; García, Beatriz; Hamacher, Duane; Montmerle, Thierry; Pasachoff, Jay; Ridpath, Ian; Sun, Xiaochun; van Gent, Robert. "Bulletin of the IAU Working Group on Star Names, No. 1" (PDF). Archived (PDF) from the original on 17 April 2018. Retrieved 28 July 2016.
- ^ Mamajek, Eric; García, Beatriz; Hamacher, Duane; Montmerle, Thierry; Pasachoff, Jay; Ridpath, Ian; Sun, Xiaochun; van Gent, Robert (July 2016). "IAU Catalog of Star Names". Archived from the original on 7 July 2018. Retrieved 28 July 2016.
- ^ "IAU Catalog of Star Names (IAU-CSN)". Archived from the original on 2018-07-07. Retrieved 2016-08-14 – via www.pas.rochester.edu.
- ^ Schaaf 2008, p. 155.
- ^ a b Schaaf 2008, p. 152.
- Bibcode:1998JBAA..108....9R.
- ^ a b c d Allen 2013, p. 88.
- ^ a b Allen 2013, p. 86.
- S2CID 162239618.
- doi:10.1086/140625.
- Bibcode:1899Obs....22..436N.
- from the original on 2020-05-29. Retrieved 2019-08-27.
- ^ (PDF) from the original on 2017-08-13. Retrieved 2018-11-04.
- S2CID 120643829.
- doi:10.1086/142551.
- ^ Tubbs, Bob (April 1997). "Modern Optical Interferometry". Archived from the original on 2017-04-20. Retrieved 19 April 2017.
- doi:10.1086/116995. See §1 for spectral types, Table 1 for orbit, Table 5 for stellar parameters, and §6.3 for the age of the system.
- Bibcode:1996A&A...306L..13B..
- doi:10.1002/asna.19141971103. 4715. Archivedfrom the original on 2020-11-05. Retrieved 2020-09-30.
- doi:10.1086/105349..
- doi:10.1086/143788.
- doi:10.1086/147742.
- ^ Philip A. Charles and Frederick D. Seward, Exploring the X-Ray Universe (Cambridge University Press, 1995) p.7
- ^ doi:10.1086/181741.
- S2CID 119444967.
- S2CID 119509015.
- ^ Schaaf 2008, p. 146.
- ^ Burnham 1978, p. 261.
- ISBN 978-0-7503-0654-6. Archivedfrom the original on 2017-03-28. Retrieved 2017-03-27.
- ISBN 978-1-107-42743-3. Archivedfrom the original on 2020-07-25. Retrieved 2020-05-27.
- ^ Ridpath & Tirion 2001, pp. 86–88.
- S2CID 59039482. A35.
- Bibcode:1998S&T....95d..59T. – based on computations from Hipparcos data. (The calculations exclude stars whose distance or proper motion is uncertain.) [1] [2] Archived 2020-05-28 at the Wayback Machine
- ^ .
- ^ Schaaf 2008, p. 154.
- ^ a b Ayres, Thomas R. (1984). "Capella HL". Cool Stars, Stellar Systems, and the Sun: Capella HL. Lecture Notes in Physics. Vol. 193. p. 202. )
- ^ a b Burnham 1978, p. 264.
- Bibcode:2014yCat....1.2023S.
- ^ S2CID 119184231.
- S2CID 118803592.
- ^ Schaaf 2008, pp. 153–55.
- .
- ^ a b
doi:10.1086/153340.
- ^ a b
Bibcode:1975ascp.book.....H.
- ^
Gontcharov, G.A. (2012). "Spatial distribution and kinematics of OB stars". Astronomy Letters. 38 (11): 694–706. S2CID 119108982.
- ^ S2CID 118365710.
- S2CID 954298.
- ^
Schlimmer, J. (2010). "Double star measurements using a webcam". Journal of Double Star Observations. Annual Report of 2009. 6 (3): 197. Bibcode:2010JDSO....6..197S.
- ^
Shaya, Ed J.; Olling, Rob P. (2011). "Very wide binaries and other co-moving stellar companions: A Bayesian analysis of the Hipparcos catalogue". The Astrophysical Journal Supplement. 192 (1): 2. S2CID 119226823.
- ^
Hełminiak, K.G.; Konacki, M.; Kulkarni, S.R.; Eisner, J. (2009). "Precision astrometry of a sample of speckle binaries and multiples with the adaptive optics facilities at the Hale and Keck II telescopes". Monthly Notices of the Royal Astronomical Society. 400 (1): 406–421. S2CID 14169943.
- ISBN 978-0-939923-78-6.
- ^ Winterburn 2009, p. 131.
- ^ Ridpath, Ian. "Auriga". Star Tales. self-published. Retrieved 30 March 2022.
- ^ a b c Allen 2013, p. 87.
- ^ Edward William Lane's Arabic-English Lexicon: cwq
- S2CID 131527348.
- S2CID 117470993.
- Bibcode:2008POBeo..85...97C.
- ISBN 978-1-4655-7650-7. Archivedfrom the original on 2017-03-13. Retrieved 2017-03-13.
- ISBN 978-3-87667-021-8. Archivedfrom the original on 2017-03-13. Retrieved 2017-03-13.
- ^ "AEEA 天文教育資訊網, Activities of Exhibition and Education in Astronomy" (in Chinese). National Museum of Natural Science, Taiwan. Archived from the original on 16 July 2011. Retrieved 31 December 2008.
- ISBN 978-0-387-95310-6.
- ^ "香港太空 館 – 研究資源 – 亮星中英對照表 (Chinese/English Star names)" (in Chinese). Hong Kong Space Museum. Archived from the original on 29 September 2009. Retrieved 31 December 2008.
- Bibcode:1942LAstr..56..137A.
- JSTOR 20700813.
- ISBN 978-0-88854-427-8.
- from the original on 2018-07-20. Retrieved 2017-06-22.
- Bibcode:1857PPIVT...2..137S.
- ISBN 978-0-9750908-0-0.
Sources
- ISBN 978-0-486-13766-7.
- ISBN 978-0-486-23567-7.
- ISBN 978-0-691-08913-3.
- ISBN 978-1-4020-8319-8.
- Schaaf, Fred (2008). The Brightest Stars: Discovering the Universe through the Sky's Most Brilliant Stars. Wiley. ISBN 978-0-470-24917-8.
- Winterburn, Emily (2009). The Stargazer's Guide: How to Read Our Night Sky. Harper Perennial. ISBN 978-0-06-178969-4.