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== Nomenclature == |
== Nomenclature == |
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''Beta Orionis'' is the star's [[Bayer designation]]. The traditional name ''Rigel'' is first recorded in the [[Alfonsine Tables]] of 1252. It is derived from the Arabic name ''{{transl|ar|Rijl Jauzah al Yusrā}}'', "the left leg (foot) of Jauzah" (i.e. ''rijl'' meaning "leg, foot"),<ref name=allen/> which can be traced to the 10th century.<ref name="KUNITZSCH1959"/> "Jauzah" was a proper name of the Orion figure, an alternative Arabic name was {{lang|ar|رجل الجبار}} ''{{transl|ar|riǧl al-ǧabbār}}'', "the foot of the great one", which is the source of the rarely used variant names ''Algebar'' or ''Elgebar''. The ''Alphonsine Tables'' saw its name split into "Rigel" and "Algebar", with the note, "et dicitur Algebar. Nominatur etiam Rigel."<ref name=Kunitzsch86/> Alternate spellings from the 17th century include ''Regel'' by Italian astronomer [[Giovanni Battista Riccioli]], ''Riglon'' by German astronomer [[Wilhelm Schickard]], and ''Rigel Algeuze'' or ''Algibbar'' by English scholar [[Edmund Chilmead]].<ref name="allen"/> |
''Beta Orionis'' is the star's [[Bayer designation]]. The traditional name ''Rigel'' is first recorded in the [[Alfonsine Tables]] of 1252. It is derived from the Arabic name ''{{transl|ar|Rijl Jauzah al Yusrā}}'', "the left leg (foot) of Jauzah" (i.e. ''rijl'' meaning "leg, foot"),<ref name=allen/> which can be traced to the 10th century.<ref name="KUNITZSCH1959"/> "Jauzah" was a proper name of the Orion figure, an alternative Arabic name was {{lang|ar|رجل الجبار}} ''{{transl|ar|riǧl al-ǧabbār}}'', "the foot of the great one", which is the source of the rarely used variant names ''Algebar'' or ''Elgebar''. The ''Alphonsine Tables'' saw its name split into "Rigel" and "Algebar", with the note, "et dicitur Algebar. Nominatur etiam Rigel."<ref name=Kunitzsch86/> Alternate spellings from the 17th century include ''Regel'' by Italian astronomer [[Giovanni Battista Riccioli]], ''Riglon'' by German astronomer [[Wilhelm Schickard]], and ''Rigel Algeuze'' or ''Algibbar'' by English scholar [[Edmund Chilmead]].<ref name="allen"/> |
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Although Rigel is a variable star, it does not have a separate [[variable star designation]] because it has a Bayer designation.<ref name=gcvs/> |
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In 2016, the [[International Astronomical Union]] organized a [[IAU Working Group on Star Names|Working Group on Star Names]] (WGSN)<ref name="WGSN"/> to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016<ref name="WGSN1"/> included a table of the first two batches of names approved by the WGSN, which included ''Rigel'' for the star β Orionis A. It is now so entered in the IAU Catalog of Star Names.<ref name="IAU-CSN"/> |
In 2016, the [[International Astronomical Union]] organized a [[IAU Working Group on Star Names|Working Group on Star Names]] (WGSN)<ref name="WGSN"/> to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016<ref name="WGSN1"/> included a table of the first two batches of names approved by the WGSN, which included ''Rigel'' for the star β Orionis A. It is now so entered in the IAU Catalog of Star Names.<ref name="IAU-CSN"/> |
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==Observation== |
==Observation== |
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The apparent visual magnitude of Rigel is 0.13, making it on average the seventh-brightest star in the [[celestial sphere]] excluding the Sun—just fainter than [[Capella (star)|Capella]]. It is an irregular [[pulsating variable]] with a visual range of magnitude 0.05–0.18. Although Rigel has the [[Bayer designation]] "beta", it is almost always brighter than Alpha Orionis ([[Betelgeuse]]). |
The apparent visual magnitude of Rigel is 0.13, making it on average the seventh-brightest star in the [[celestial sphere]] excluding the Sun—just fainter than [[Capella (star)|Capella]]. It is an irregular [[pulsating variable]] with a visual range of magnitude 0.05–0.18. Although Rigel has the [[Bayer designation]] "beta", it is almost always brighter than Alpha Orionis ([[Betelgeuse]]). |
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Revision as of 17:31, 29 January 2019
Rigel (/ˈraɪdʒəl, -ɡəl/), also designated β Orionis (Latinized to Beta Orionis, abbreviated Beta Ori, β Ori), is on average the seventh-brightest star in the night sky and the brightest in the constellation of Orion—though occasionally it is outshone within the constellation by the variable star Betelgeuse. With an average apparent magnitude of 0.13, it is a luminous object some 863 light-years distant from Earth.
Rigel as seen from Earth is actually a multiple star system of three to five stars. A companion, Rigel B, is 500 times fainter than the supergiant Rigel A and visible only with a telescope. Rigel B is itself a multiple star system, including a spectroscopic pair and a visual companion C. Component C, with a very similar brightness and spectrum to B, is probably not the spectroscopic companion, making the system a triple star.
The primary star, Rigel A, is a blue-white supergiant estimated to be anywhere from 61,500 to 363,000 times as luminous as the Sun, depending on the method used to calculate its properties and assumptions about its distance. It has exhausted the hydrogen in its core and expanded to between 79 and 115 times the Sun's radius. It pulsates quasi-periodically and is classified as an Alpha Cygni variable.
Nomenclature
![](https://upload.wikimedia.org/wikipedia/commons/thumb/4/4a/Treasures3.jpg/220px-Treasures3.jpg)
Beta Orionis is the star's Bayer designation. The traditional name Rigel is first recorded in the Alfonsine Tables of 1252. It is derived from the Arabic name Rijl Jauzah al Yusrā, "the left leg (foot) of Jauzah" (i.e. rijl meaning "leg, foot"),[17] which can be traced to the 10th century.[18] "Jauzah" was a proper name of the Orion figure, an alternative Arabic name was رجل الجبار riǧl al-ǧabbār, "the foot of the great one", which is the source of the rarely used variant names Algebar or Elgebar. The Alphonsine Tables saw its name split into "Rigel" and "Algebar", with the note, "et dicitur Algebar. Nominatur etiam Rigel."[19] Alternate spellings from the 17th century include Regel by Italian astronomer Giovanni Battista Riccioli, Riglon by German astronomer Wilhelm Schickard, and Rigel Algeuze or Algibbar by English scholar Edmund Chilmead.[17]
Although Rigel is a variable star, it does not have a separate variable star designation because it has a Bayer designation.[20]
In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[21] to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016[22] included a table of the first two batches of names approved by the WGSN, which included Rigel for the star β Orionis A. It is now so entered in the IAU Catalog of Star Names.[23]
Observation
The apparent visual magnitude of Rigel is 0.13, making it on average the seventh-brightest star in the celestial sphere excluding the Sun—just fainter than Capella. It is an irregular pulsating variable with a visual range of magnitude 0.05–0.18. Although Rigel has the Bayer designation "beta", it is almost always brighter than Alpha Orionis (Betelgeuse).
Since 1943, the spectrum of this star has served as the spectral reference, for class B8Ia, by which other stars are classified.[24][25] Rigel has a color index (B–V) of −0.03, meaning it appears white or slightly blue-white.[26]
Culminating at midnight on 12 December, and at 9 pm on 24 January, Rigel is most visible in winter evenings in the northern hemisphere and summer in the southern.[27] In the southern hemisphere, Rigel is the first bright star of Orion visible as the constellation rises.[28]
In stellar navigation, Rigel is one of the most important navigation stars, since it is bright, easily located and equatorial, which means it is visible all around the world's oceans (the exception, areas within 8° of the North Pole).[29]
Spectroscopy
The general spectral type of Rigel as B8 is well-established and it has been used as a defining point of the spectral classification sequence for supergiants. However the details of the spectrum vary considerably owing to periodic atmospheric eruptions. The spectral lines show emission, absorption, line doubling, P Cygni profiles, and inverse P Cygni profiles, with no obvious periodicity.[30] This has resulted in classification as B8 Iab, B8 Iae, or blendings by different authors.[13][31]
Variability
Rigel has been known to vary in brightness since at least 1930, although the exact range and type of variability was unclear. Published results showed variations of less than 0.1 magnitudes with no obvious period. Observations in 1984 showed variations at red, blue, and yellow wavelengths of up to 0.13 magnitudes on timescales of a few hours to several days, but again no clear period. The colour index also varied but in general was not strongly correlated with the brightness variations.[32]
From an analysis of Hipparcos satellite photometry, Rigel was identified as belonging to the Alpha Cygni variables in 1998.[33] It was added to the General Catalogue of Variable Stars in the following year in the 74th namelist of variable stars.[34] The Hipparcos photometry showed variations with a photographic amplitude of 0.039 magnitudes and a possible period of 2.075 days.[35]
Rigel was observed with the Canadian MOST satellite for nearly 28 days in 2009. The light variations in this supergiant star were at the milli-magnitude level. The gradual changes in the flux highlights the presence of long-period pulsation modes in the star.[14]
Distance
The distance to Rigel has been difficult to determine with any accuracy, as its brightness is not easy to determine independently and its is somewhat too distant for very accurate parallax measurements. As it is both bright and moving through a region of nebulosity, Rigel lights up several dust clouds in its vicinity, most notably IC 2118 (the Witch Head Nebula).[36] Rigel has been classified as an outlying member of the Orion OB1 Association at a distance of up to 500 pc. It has also been listed as a member of the poorly-defined Taurus-Orion R1 Association, somewhat closer at 360 pc.[37][38] It is thought to be considerably closer than most of the members of Orion OB1 and the Orion Nebula, but projecting Rigel's path through space for its expected age brings it close to the nebula. Betelgeuse and Saiph lie at a similar distance to Rigel, although Betelgeuse is a runaway star with a complex history and is likely to have originally formed in the main body of the association.[31]
The revised 2007 Hipparcos reduction of Rigel's parallax gives a distance of 863 light-years (265 parsecs), with a margin of error of about 9%.[2]
A companion star to Rigel, usually considered to be physically associated and at the same distance, has a Gaia Data Release 2 parallax of 2.9186±0.0761 mas, implying a distance around 340 pc but the measurements show a number of features suggesting they may be unreliable, possibly because it is a close double star.[39]
Stellar system
Rigel has been known as a visual double star since at least 1822, when it was measured by Friedrich Georg Wilhelm von Struve.[40] The companion is not particularly faint at magnitude 6.7, and with a separation of 9.5 arc seconds both components are resolvable in most amateur astronomers' telescopes.[40] However, the large difference in brightness makes it a challenging target for telescope apertures smaller than 15.0 cm (5.9 in). The companion is frequently referred to as Rigel B, but more correctly as β Orionis B or by a multiple star designation such as ADS 3823 B.[41]
A spectroscopic companion to Rigel has been reported on the basis of radial velocity variations, and even an orbit calculated, but it is thought that the star does not exist and the pulsations are intrinsic to Rigel itself.[42]
At Rigel's estimated distance, Rigel B's projected separation from its primary is over 2,200 AU. Since its discovery, there has been no sign of orbital movement, although both stars share similar common proper motion.[42][36] The pair would have a minimum orbital period of around 18,000 years.[7] Gaia Data Release 2 (DR2) contains a somewhat unreliable parallax for Rigel B placing it at about 340 pc, further away than the Hipparcos distance for Rigel, but similar to the Taurus-Orion R1 association. There is no parallax for Rigel in Gaia DR2. The Gaia DR2 proper motions for Rigel B and the Hipparcos proper motions for Rigel are both small, although not quite the same.[39]
Since the 19th century, Rigel B has been reported to be resolved into a close binary of two equal components, with the measured separation varying from less than 0.1" to nearly 0.2". Speckle interferometry showed in 2009 two almost identical components separated by 0.124".[43] The companion is designated as component C. Both stars have apparent visual magnitudes of 7.6 with a likely orbital period of 63 years.[7]
Rigel B itself appears to be a spectroscopic binary system, consisting of two main sequence stars that orbit each other every 9.86 days. These two stars do not seem to correspond to the visual binary components of B or C, so the BC sub-system might be a triple, although the true arrangement is unclear.[42]
Multiple star catalogs include a 15th magnitude star at 44.6″ and position angle of 1°, catalogued as component D, although it is unclear whether it is physically related or a coincidental alignment.[40] Gaia DR2 finds it to be a 12th magnitude sunlike star at approximately the same distance as Rigel.[44]
Physical characteristics
Moravveji and colleagues calculate a luminosity for Rigel A of 120,000 times that of the Sun.[14] Its surface temperature is around 12,100 K. The interferometer-measured angular diameter of this star, after correction for limb darkening, is 2.75±0.01 mas.[45] At its estimated distance, this yields a size of about 78.9 times the radius of the Sun.[14] Norbert Przybilla and colleagues assumed a distance of 360 ± 40 parsecs (1,170 ± 130 light-years). They calculated it to be around 218,000 times as luminous as the Sun, and have around 21 ± 3 solar masses and 109 ± 12 times its radius.[8]
A 2018 study using the Navy Precision Optical Interferometer came up with an angular diameter of 2.606 ± 0.009 mas, yielding a radius of 74.1+6.1
−7.3 times that of the Sun, and luminosity 61515 ± 11486 times that of the Sun.[46] Based on the Hipparcos distance of 240 pc and an Orion OB1 association distance of 500 pc, the luminosity is calculated to be somewhere between 83,000 L☉ and 363,000 L☉[37]
Rigel A is a blue supergiant that has exhausted burning the hydrogen fuel in its core and left the main sequence, expanding and brightening as it progresses across the Hertzsprung–Russell diagram. Przybilla estimated that it has lost around 3 solar masses since beginning life as a star of 24 ± 3 solar masses 7 to 9 million years ago.[8] It will become a red supergiant and eventually end its stellar life by exploding as a type II supernova, in the process flinging out material that will serve to seed future generations of stars.[10] It is one of the closest known potential supernova progenitors to Earth,[14] and would be expected to have an apparent magnitude of around −11 at its peak.[4]
Rigel's variability is complex and is caused by stellar pulsations similar to those of Deneb, the prototype of the class of Alpha Cygni pulsating stars. The radial velocity variations of Rigel prove that it simultaneously oscillates in at least 19 non-radial modes with periods ranging from about 1.2 to 74 days.[14] While its pulsations are powered by the nuclear reactions in a hydrogen-burning shell that is at least partially non-convective, the star also burns helium in its core.[10]
The companions Rigel Ba, Bb, and C all appear to be similar B class main sequence stars of 3 - 4 M☉, but their properties are not accurately known.[7]
Etymology and cultural significance
In ancient Egypt, Rigel's is thought to have been called Seba-en-Sah Sb3-n-S3ḥ, which means Star of Sah.[47] In heiroglyphics:
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Rigel is presumably the star known as "Aurvandil's toe" in Norse mythology.[48]
In Chinese, 參宿 (Shēn Sù), meaning Three Stars (asterism), refers to an asterism consisting of Rigel, Alnitak, Alnilam, Mintaka, Betelgeuse, Bellatrix and Saiph.[49] Consequently, Rigel are known as 參宿七 (Shēn Sù qī, English: the Seventh Star of Three Stars).[50]
In Japan, the Minamoto or Genji clan chose Rigel and its white color as its symbol, calling the star Genji-boshi (源氏星), while the Taira or Heike clan adopted Betelgeuse and its red color. The two powerful families fought a legendary war in Japanese history, the stars seen as facing each other off and only kept apart by the Belt.[51][52][53] Rigel was also known as Gin-waki, (銀脇), "the Silver (Star) beside (Mitsu-boshi)".
Rigel was known as Yerrerdet-kurrk to the Wotjobaluk koori of southeastern Australia, and held to be the mother-in-law of Totyerguil (Altair). The distance between them signified the taboo preventing a man from approaching his mother-in-law.[54] The indigenous Boorong people of northwestern Victoria named Rigel as Collowgullouric Warepil.[55] The Wardaman people of northern Australia know Rigel as the Red Kangaroo Leader Unumburrgu and chief conductor of ceremonies in a songline when Orion is high in the sky. The river Eridanus marks a line of stars in the sky leading to it, and the other stars of Orion are his ceremonial tools and entourage. Betelgeuse is Ya-jungin "Owl Eyes Flicking", watching the ceremonies.[56]
The Māori people named Rigel as Puanga, which was said to be a daughter of Rehua (Antares), the chief of all stars.[57] Its heliacal rising also presaged the appearance of Matariki (the Pleiades) in the dawn sky which marked the Māori New Year in late May or early June. The Moriori people of the Chatham Islands, as well as some Maori groups in New Zealand, marked the start of their New Year with Rigel rather than the Pleiades.[58] Puaka was a local variant used in the South Island.[59]
The Lacandon people of southern Mexico knew it as tunsel ("little woodpecker").[60]
In modern culture
The MS Rigel was originally a Norwegian ship, built in Copenhagen in 1924. It was requisitioned by the Germans during the second World War and sunk in 1944 while being used to transport prisoners of war.
The name, or the star itself, also occurs frequently in fictional works.
References
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- ^ a b c d e f van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357.
- ^ Ducati, 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.
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- ^ a b DENIS Consortium (2005). "VizieR Online Data Catalog: The DENIS database (DENIS Consortium, 2005)". VizieR On-line Data Catalog: B/denis. Originally published in: 2005yCat.2263....0T. 1. Bibcode:2005yCat....102002D.
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{{cite book}}
: CS1 maint: multiple names: authors list (link) - ^ a b c "Spectroscopic Binary Catalogue (SB9)". D.Pourbaix. Retrieved 13 March 2016.
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- ^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ Aufdenberg, J. P.; et al. (2008). "Limb Darkening: Getting Warmer". The Power of Optical/IR Interferometry. Eso Astrophysics Symposia. 1 (1): 71–82. Bibcode:2008poii.conf...71A. doi:10.1007/978-3-540-74256-2_8. ISBN 978-3-540-74253-1.
- ^ Baines, Ellyn K.; Armstrong, J. Thomas; Schmitt, Henrique R.; Zavala, R. T.; Benson, James A.; Hutter, Donald J.; Tycner, Christopher;; van Belle, Gerard T. (2017). "Fundamental parameters of 87 stars from the Navy Precision Optical Interferometer". The Astronomical Journal. 155 (1): 16. Bibcode:2018AJ....155...30B. doi:10.3847/1538-3881/aa9d8b.
{{cite journal}}
: CS1 maint: extra punctuation (link) CS1 maint: multiple names: authors list (link) CS1 maint: unflagged free DOI (link) - ^ Lull, José; Belmonte, Juan Antonio (2009). The constellations of ancient Egypt. Bibcode:2009iscc.book..155L.
- ^ Richard Cleasby; Gudbrand Vigfusson (1874). An Icelandic-English Dictionary. Clarendon Press.
- ^ 陳久金 (2005). 中國星座神話 (in Chinese). 台灣書房出版有限公司. ISBN 978-986-7332-25-7.
- ^ "天文教育資訊網" [AEEA (Activities of Exhibition and Education in Astronomy)] (in Chinese). 2006-05-25.
- ^ Steve Renshaw; Saori Ihara (October 1999). "Yowatashi Boshi; Stars that Pass in the Night". Griffith Observer. Archived from the original on 2 January 2013. Retrieved 25 June 2012.
{{cite web}}
: Unknown parameter|deadurl=
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suggested) (help); Unknown parameter|last-author-amp=
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suggested) (help) - ^ "Daijirin. Sanseido. 1990. p. 181.
- ^ Hōei Nojiri. Shin seiza jyunrei. p. 19. ISBN 978-4-12-204128-8.
- ^ Mudrooroo (1994). Aboriginal mythology : an A-Z spanning the history of aboriginal mythology from the earliest legends to the present day. London: HarperCollins. p. 142. ISBN 978-1-85538-306-7.
- ^ Hamacher, Duane W.; Frew, David J. (2010). "An Aboriginal Australian Record of the Great Eruption of Eta Carinae". Journal of Astronomical History & Heritage. 13 (3): 220–34. arXiv:1010.4610. Bibcode:2010JAHH...13..220H.
- ^ Harney, Bill Yidumduma; Cairns, Hugh C. (2004) [2003]. Dark Sparklers (Revised ed.). Merimbula, New South Wales: Hugh C. Cairns. pp. 139–40. ISBN 0-9750908-0-1.
- ^ Janet Parker; Alice Mills; Julie Stanton (2007). Mythology: Myths, Legends and Fantasies. Durban, Struik Publishers. p. 419,.
{{cite book}}
: CS1 maint: extra punctuation (link) - ^ Kelley, David H.; Milone, Eugene F. (2011). Exploring Ancient Skies: A Survey of Ancient and Cultural Astronomy. Springer. p. 341. ISBN 144197623X.
- ^ Best, Elsdon (1922). Astronomical Knowledge of the Maori: Genuine and Empirical. Wellington, New Zealand: Dominion Museum. pp. 39–40.
- ^ Milbrath, Susan (1999). Star Gods of the Maya: Astronomy in Art, Folklore, and Calendars. Austin, Texas: University of Texas Press. p. 39. ISBN 0292752261.
External links
- NASA Astronomy Picture of the Day: Rigel and the Witch Head Nebula (2018 January 15)
- NASA Astronomy Picture of the Day: A Blazing Fireball between the Orion Nebula and Rigel (2015 November 16)
- December double star of the month – beta Orionis Astronomical Society of Southern Africa
- My Favorite Double Star AAVSO