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'''Rigel''' ({{IPAc-en|ˈ|r|aɪ|dʒ|əl|,_|-|g|əl}}), also designated '''β Orionis''' ([[Latinisation of names|Latinized]] to '''Beta Orionis''', abbreviated '''Beta Ori''', '''β Ori'''), is a [[variable star]]. It is, on average, the [[list of brightest stars|seventh-brightest star]] in the [[night sky]] and the brightest star in the [[constellation]] of [[Orion (constellation)|Orion]]—though occasionally it is outshone within the constellation by [[Betelgeuse]], another variable star. The [[apparent magnitude]] of Rigel varies irregularly between +0.05 and +0.18.
'''Rigel''' ({{IPAc-en|ˈ|r|aɪ|dʒ|əl|,_|-|g|əl}}), also designated '''β Orionis''' ([[Latinisation of names|Latinized]] to '''Beta Orionis''', abbreviated '''Beta Ori''', '''β Ori'''), is a [[variable star]]. It is, on average, the [[list of brightest stars|seventh-brightest star]] in the [[night sky]] and the brightest star in the [[constellation]] of [[Orion (constellation)|Orion]]—though occasionally it is outshone within the constellation by [[Betelgeuse]], another variable star. The [[apparent magnitude]] of Rigel varies irregularly between +0.05 and +0.18.


Although appearing as a single star to the naked eye, Rigel is actually part of a multiple [[star system]]. The name ''Rigel'' strictly refers to only the brightest component, although it is commonly applied to the whole system. It is a [[Massive star|massive]] [[blue-white supergiant]] estimated to be anywhere from 61,500 to 363,000 times [[Solar luminosity|as luminous as the Sun]], depending on the method used to calculate its properties and assumptions about its distance, estimated to be about {{convert|860|ly|pc|sigfig=2}}. Rigel's radius is over 70 times that of the [[Solar radius|Sun]]. Pulsations cause Rigel's small intrinsic brightness variations and it is classified as an [[Alpha Cygni variable]]. Rigel's physical parameters are poorly known, and its rapid complex evolution is not well understood, though the star's likely fate in the future is to end as a [[supernova]].
Although appearing as a single star to the naked eye, Rigel is actually part of a multiple [[star system]]. The name ''Rigel'' strictly refers to only the brightest component, although it is commonly applied to the whole system. It is a [[Massive star|massive]] [[blue-white supergiant]] estimated to be anywhere from 61,500 to 363,000 times [[Solar luminosity|as luminous as the Sun]], depending on the method used to calculate its properties and assumptions about its distance, estimated to be about {{convert|860|ly|pc|sigfig=2}}. Rigel's radius is over 70 times that of the [[Solar radius|Sun]]. Pulsations cause Rigel's small intrinsic brightness variations and it is classified as an [[Alpha Cygni variable]]. Rigel's physical parameters are poorly known, and its rapid complex evolution is not well understood, though the star's likely fate in the future is to end as a [[supernova]].


Separated from Rigel by {{val|9.5|ul="}}, two companion stars, Rigel B and Rigel C, are very close to each other and approximately equal in brightness. They are a [[Visual double star|visual pair]] that can be resolved by a moderately sized telescope. Together they have a combined apparent magnitude of 6.7 or 400 times fainter than the supergiant primary star. Rigel B is itself a much closer [[spectroscopic binary]], with components Ba and Bb that are separated by less than {{val|1|ul=mas}}.
Rigel appears as a [[Visual double star|visual pair]] that can be resolved by small to moderate sized telescopes. The much fainter 6.7 [[apparent magnitude|magnitude]] companion, known as Rigel B, is separated from Rigel by {{val|9.5|ul="}}, but is often difficult to view as it is 400 times fainter than the primary star. Rigel B forms another very close double star with Rigel C, whose components are approximately equal in brightness. Star Rigel B is again a much closer unresolved [[spectroscopic binary]] (Rigel Ba and Rigel Bb) that are separated by less than {{val|1|ul=mas}}. These stars together may form a physical triple star orbiting its bright supergiant primary.


== Nomenclature ==
== Nomenclature ==

Revision as of 23:48, 12 April 2019

For other uses, see Rigel (disambiguation).
Rigel
Map of the constellation Orion
Rigel in the constellation Orion (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Orion
Pronunciation /ˈraɪdʒəl/ or /-ɡəl/[1]
A
Right ascension 05h 14m 32.27210s[2]
Declination −08° 12′ 05.8981″[2]
Apparent magnitude (V) 0.13[3] (0.05–0.18[4])
BC
Right ascension 05h 14m 32.049s[5]
Declination −08° 12′ 14.78″[5]
Apparent magnitude (V) 6.67[6] (7.6/7.6[7])
Characteristics
A
Evolutionary stage Blue supergiant
Spectral type B8 Ia[8]
U−B color index −0.66[9]
B−V color index −0.03[9]
Variable type Alpha Cygni[10]
BC
Evolutionary stage Main sequence
Spectral type B9V + B9V[7]
Astrometry
Radial velocity (Rv)17.8±0.4[11] km/s
Proper motion (μ) RA: +1.31[2] mas/yr
Dec.: +0.50[2] mas/yr
Parallax (π)3.78 ± 0.34 mas[2]
Distance860 ± 80 ly
(260 ± 20 pc)
Absolute magnitude (MV)–7.84[12]
Orbit[6]
PrimaryBa
CompanionBb
Period (P)9.860 days
Eccentricity (e)0.1
Semi-amplitude (K1)
(primary)		25.0 km/s
Semi-amplitude (K2)
(secondary)		32.6 km/s
Orbit[7]
PrimaryB
CompanionC
Period (P)63 yr
Details
A
Mass21±3[13] M☉
Radius78.9±7.4[14] R☉
Luminosity (bolometric)1.20+0.25
−0.21×105[14] L☉
Surface gravity (log g)1.75±0.10[15] cgs
Temperature12100±150[15] K
Metallicity [Fe/H]−0.06±0.10[8] dex
Rotational velocity (v sin i)25±3[15] km/s
Age8±1[8] Myr
Ba
Mass3.84[7] M☉
Bb
Mass2.94[7] M☉
C
Mass3.84[7] M☉
Other designations
β Orionis, STF 668, H II 33, ADS 3823[16], CCDM J05145-0812, WDS J05145-0812[17]
A: Rigel, Algebar, Elgebar, 19 Orionis, HD 34085, HR 1713, HIP 24436, SAO 131907, BD-08°1063, FK5 194
B: Rigel B, GCRV 3111, STF 688B, BU 555B
Database references
SIMBADdata

Rigel (/ˈraɪdʒəl, -ɡəl/), also designated β Orionis (Latinized to Beta Orionis, abbreviated Beta Ori, β Ori), is a variable star. It is, on average, the seventh-brightest star in the night sky and the brightest star in the constellation of Orion—though occasionally it is outshone within the constellation by Betelgeuse, another variable star. The apparent magnitude of Rigel varies irregularly between +0.05 and +0.18.

Although appearing as a single star to the naked eye, Rigel is actually part of a multiple star system. The name Rigel strictly refers to only the brightest component, although it is commonly applied to the whole system. It is a massive 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, estimated to be about 860 light-years (260 pc). Rigel's radius is over 70 times that of the Sun. Pulsations cause Rigel's small intrinsic brightness variations and it is classified as an Alpha Cygni variable. Rigel's physical parameters are poorly known, and its rapid complex evolution is not well understood, though the star's likely fate in the future is to end as a supernova.

Rigel appears as a visual pair that can be resolved by small to moderate sized telescopes. The much fainter 6.7 magnitude companion, known as Rigel B, is separated from Rigel by 9.5″, but is often difficult to view as it is 400 times fainter than the primary star. Rigel B forms another very close double star with Rigel C, whose components are approximately equal in brightness. Star Rigel B is again a much closer unresolved spectroscopic binary (Rigel Ba and Rigel Bb) that are separated by less than 1 mas. These stars together may form a physical triple star orbiting its bright supergiant primary.

Nomenclature

The earliest known recording of the modern name Rigel is in the Alfonsine Tables of 1521. It is derived from the Arabic name Rijl Jauzah al Yusrā, "the left leg (foot) of Jauzah" (i.e. rijl meaning "leg, foot"),[18] which can be traced to the 10th century.[19] "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.[20] 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.[18] In 2016, the International Astronomical Union (IAU) officially recognized Rigel for β Orionis A[21][22], the blue supergiant component visible to the naked eye.

β Orionis (Latinized to Beta Orionis) is the star's designation given by Johann Bayer in 1603. Although Rigel has the designation beta, it is almost always brighter than Alpha Orionis (Betelgeuse).[23] Astronomer James B. Kaler has speculated that Rigel was designated by Bayer during a rare period when it was outshone by the variable star Betelgeuse, resulting in the latter star being designated alpha and Rigel designated beta.[24] Rigel is included in the General Catalogue of Variable Stars, but since it already has a Bayer designation, β Orionis, it has no separate variable star designation.[25]

Rigel has several other alternate stellar designations taken from various catalogues, including the Flamsteed designation 19 Orionis (19 Ori), the Bright Star Catalogue entry HR 1713, and the Henry Draper Catalogue number HD 34085. These designations are often seen in scientific literature,[26][13][7] but rarely in more popular writing.[27][28]

Rigel is included in many older astronomical catalogs and books as the visual double stars H II 33 or Σ 668 and β 555. For simplicity, Rigel's companions can be designated as Rigel B,[22], C, and D;[27][24] the IAU describes such names as "useful nicknames" that are "unofficial".[22] Alternative designations from the Washington Double Star Catalog are double stars: STF 668A,BC, BU 555AD, BU 555BC.[29][22], and as individual stars: STF 688B[17] for Rigel B, as BU 555Ba, BU555Bb, BC 555C and BU 555D for Rigel Ba, Bb, C and D respectively.[30][31] The whole multiple star system is known as WDS 05145-0812 or CCDM 05145-0812.

Observation

Rigel is typically the seventh-brightest star in the celestial sphere excluding the Sun. It is usually fainter than Capella,[23] although both are slightly variable in brightness. Rigel is an irregular pulsating variable with a range in apparent magnitude from 0.05 to 0.18.[4] Since 1943, the spectrum of this star has served as a reference for class B8Ia, for use as a comparison when classifying the spectra of other stars.[32][33] Rigel appears slightly blue-white, almost white, and has a (B–V) color index of −0.06.[34]

Culminating at midnight on 12 December, and at 9 pm on 24 January, Rigel is visible in winter evenings in the northern hemisphere and summer in the southern.[23] In the southern hemisphere, Rigel is the first bright star of Orion visible as the constellation rises.[35] The star is a vertex of the "Winter Hexagon", an asterism that includes Aldebaran, Capella, Pollux, Procyon, and Sirius. Rigel is a prominent equatorial navigation star, being easily located and readily visible in all the world's oceans (the exception is the area within 8° of the North Pole).[36]

Spectroscopy

Bright points of light against a dark background with wisps of coloured nebulosity
Orion with Rigel at bottom right, at optical wavelengths plus Hα to emphasize gas clouds

The general spectral type of Rigel as B8 is well-established, and it is a defining point of the spectral classification sequence for supergiants.[37][38] The overall spectrum is typical for a late B class star, with strong absorption lines of the hydrogen Balmer series together with neutral helium lines and some of heavier elements such as oxygen, calcium, and magnesium.[39] The luminosity class for B8 stars is estimated from the strength and narrowness of the hydrogen spectral lines, and Rigel is assigned to the bright supergiant class Ia.[32]

As early as 1888, the radial velocity of Rigel, as estimated from the Doppler shifts of its spectral lines, was seen to vary. This was confirmed and interpreted as due to a spectroscopic companion with a period of about 22 days.[40] The radial velocity has since been measured to vary by about 10 km/s around a mean of 21.5 km/s.[41]

In 1933, the Hα spectral line was seen to be unusually weak and shifted 0.1 nm towards shorter wavelengths, while there was a narrow emission spike about 1.5 nm to the long wavelength side of the main absorption line.[42] This is now known as a P Cygni profile after a star that shows this feature strongly in its spectrum. It is associated with mass loss where there is simultaneously emission from dense wind close to the star and absorption from circumstellar material expanding away from the star.[42]

The unusual Hα line profile is observed to vary unpredictably: around a third of the time it is a normal absorption line; about a quarter of the time it is a double-peaked line, that is an absorption line with an emission core or an emission line with an absorption core; about a quarter of the time it has a P Cygni profile; most of the rest of the time the line has an inverse P Cygni profile, where the emission component is on the short wavelength side of the line; rarely there is a pure emission Hα line.[41] The line profile changes are interpreted as variations in the quantity and velocity of material being expelled from the star. Occasional very high-velocity outflows have been inferred, and, more rarely, infalling material. The overall picture is one of large looping structures arising from the photosphere and driven by magnetic fields.[43]

Variations in the spectrum have resulted in the assignment of different classes to Rigel, such as B8 Ia, B8 Iab, and B8 Iae.[13][44]

Variability

Rigel has been known to vary in brightness since at least 1930. The range of Rigel's brightness variation is on average around 0.1 magnitudes, and this variation has no obvious period. Observations over 18 nights 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. Rigel's colour index varies but is not strongly correlated with its brightness variations.[45]

From an analysis of Hipparcos satellite photometry, Rigel was identified as belonging to the Alpha Cygni class of variable stars in 1998,[46] which is defined as "non-radially pulsating supergiants of the Bep–AepIa spectral types".[47] (The 'e' indicates it displays emission lines in the spectrum, while the 'p' means it has an unspecified spectral peculiarity.) It was added to the General Catalogue of Variable Stars in the following year in the 74th namelist of variable stars.[48] The Hipparcos photometry showed variations with a photographic amplitude of 0.039 magnitudes and a possible period of 2.075 days.[49]

Rigel was observed with the Canadian MOST satellite for nearly 28 days in 2009. Milli-magnitude variations were observed, and gradual changes in flux suggests the presence of long-period pulsation modes.[14]

Mass loss

From observations of the variable Hα spectral line, the mass loss from Rigel is estimated to be (1.5±0.4)×10−7 solar masses per year (M☉/yr), around ten million times more than the mass loss from the Sun.[50] More detailed optical and K band infrared spectroscopic observations, together with VLTI interferometry, were taken from 2006 to 2010. Analysis of the Hα and Hγ line profiles, and measurement of the regions producing the lines, show that the stellar wind varies greatly in structure and strength. Loop and arm structures were also detected within the wind. Calculations of mass loss from the Hγ line give (9.4±0.9)×10−7 M☉/yr in 2006-7 and (7.6±1.1)×10−7 M☉/yr in 2009–10. Calculations using the Hα line give lower results, around 1.5×10−7 M☉/yr. The terminal wind velocity is 300 km·s−1.[51] It is estimated that Rigel has lost around 3 solar masses since beginning life as a star of 24±3 solar masses 7 to 9 million years ago.[8]

Distance

A very bright blue-white star with fainter stars near a sharply-defined strip of nebulosity
Rigel and reflection nebula IC 2118 in Eridanus. Rigel B is not visible in the glare of the main star.

Rigel's distance from the Sun is difficult to estimate directly due to its brightness and small parallax; therefore, indirect distance estimation methods have been employed. For example, Rigel is believed to be moving through a region of nebulosity whose brightness lights up several dust clouds in its vicinity. Most notable of these is the 5°[52]–long IC 2118 (the Witch Head Nebula),[53] located at an angular separation of 2.5° from the star,[52] or a distance of 39 light-years (12 parsecs) away.[24] From measures of other nebula-embedded stars, Rigel's distance is estimated to be 949 ± 7 light-years (291 ± 2 parsecs).[54]

Rigel is an outlying member of the Orion OB1 Association, which is located at a distance of up to 1,600 light-years (500 parsecs) from Earth. It is a member of the loosely-defined Taurus-Orion R1 Association, somewhat closer at 1,200 light-years (360 parsecs).[26][55] Rigel is thought to be considerably closer than most of the members of Orion OB1 and the Orion Nebula. Betelgeuse and Saiph lie at a similar distance to Rigel, although Betelgeuse is a runaway star with a complex history and might have originally formed in the main body of the association.[44]

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, suggesting a distance around 1,100 light-years (340 parsecs). However, the measurements for this object may be unreliable, possibly because it is a close double star.[56]

Stellar system

Rigel
Separation=9.5″
Period=24,000 y
Ba
Separation=0.58 mas
Period=9.860 d
Bb
Separation=0.1″
Period=63 y
C

Hierarchical scheme for Rigel's components[7]

The Rigel star system has at least four components. The blue supergiant primary has a visual companion which is itself a likely close triple star. A more distant visual companion might be a part of the Rigel system.

William Herschel discovered Rigel to be a visual double star on 1 October 1781, and it was catalogued as H II 33 (or H 2 33[29]).[57] Friedrich Georg Wilhelm von Struve first measured the relative position of the companion in 1822, cataloging the visual pair as Σ 668.[58] The secondary star can be referred to as Rigel B or β Ori B. The angular separation of Rigel B from the primary star is 9.5 arc seconds to its south along position angle 204°.[29][59] Although not particularly faint at visual magnitude 6.7, the overall difference in brightness from the primary (about 6.6 magnitudes or 440 times fainter) makes it a challenging target for telescope apertures smaller than 15 cm (6 in).[6]

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 motion, although both stars share similar common proper motion.[60][53] 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 1,100 light-years (340 parsecs), 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.[56]

In 1871, Sherburne Wesley Burnham suspected Rigel B to be double, and in 1878, he resolved it into two components .[61] The two stars were measured at an equally bright visual magnitude 7.6.[6] This visual companion is designated as component C (Rigel C), with a measured separation from component B that varies from less than 0.1″ to around 0.3″.[29][61] In 2009, speckle interferometry showed two almost identical components separated by 0.124".[62]. Their estimated orbital period is 63 years.[7]

Rigel B appears to be a double-lined spectroscopic binary system (Rigel Ba, Bb), with the individual absorption lines of both components visible in the spectrum. The pair consists of two main sequence stars that orbit each other every 9.86 days. This spectroscopic binary along with the close visual component Rigel C is likely a physical triple star system.[60][6]

In 1878, Burnham found another possibly associated star of approximately 13th magnitude, catalogued as component D.[61] (Rigel D). Its 2017 separation from Rigel was 44.5″ almost due north at position angle of 1°,[29] although it is unclear whether it is physically related or a coincidental alignment. Gaia DR2 finds it to be a 12th magnitude sunlike star at approximately the same distance as Rigel.[63] Likely an orange dwarf, this star would have an orbital period of around 250,000 years, if it is part of the Rigel system.[24]

A spectroscopic companion to Rigel was reported on the basis of radial velocity variations, and its orbit was even calculated, but subsequent work suggests that the star does not exist and that observed pulsations are intrinsic to Rigel itself.[60]

Physical characteristics

A chart showing several labelled stars against shaded coloured areas with axes of spectral type and absolute magnitude
Rigel's place at top center on the Hertzsprung-Russell diagram

Estimation of many physical characteristics of Rigel and other blue supergiant stars are difficult due to their rarity and uncertainty about how far they are from the Sun. As such, much of our understanding about their characteristics is based on theoretical stellar evolution models.

Although Rigel is often considered the most luminous star within 1,000 light-years of the Sun,[28][23] its energy output is poorly known. For example, using the Hipparcos distance of 860 light-years (264 parsecs), the estimated relative luminosity for Rigel is about 120,000 times that of the Sun,[14] but another recently published distance of 1,170 ± 130 light-years (360 ± 40 parsecs) suggests an even higher luminosity of 218,000 times that of the Sun. Other calculations based on theoretical stellar evolutionary models of Rigel's atmosphere give luminosities anywhere between 83,000 L☉ and 363,000 L☉,[26] while summing the spectral energy distribution from historical photometry with the Hipparcos distance suggests a luminosity as low as 61,515±11,486 L☉.[64]

A 2018 study using the Navy Precision Optical Interferometer measured the angular diameter as 2.526 mas. After correcting for limb darkening, the angular diameter is found to be 2.606±0.009 mas, yielding a radius of 74.1+6.1
−7.3 R☉.[64] An older measurement of the angular diameter gives 2.75±0.01 mas,[65] equivalent to a radius 78.9 times the radius of the Sun (R☉) at 264 pc.[14]

A mass of 21±3 M☉ at an age of 8±1million years has been determined by comparing evolutionary tracks , while atmospheric modelling from the spectrum gives a mass of 24±8 M☉.[8] From the spectral type and colour, Rigel's surface temperature is estimated to be about 12,100 K.[15]

Rigel is a blue supergiant that has exhausted the hydrogen fuel in its core, evolved away from the main sequence and expanded as it has progressed across the Hertzsprung–Russell diagram.[66] Its pulsation properties suggest it may have already passed through the red supergiant phase, although the surface abundances are only compatible with this if certain assumptions are made about internal convection.[67] Rigel is expected to eventually end its stellar life as a 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 complex variability at visual wavelengths is caused by stellar pulsations similar to those of Deneb. Additional observations of radial velocity variations indicates that it simultaneously oscillates in at least 19 non-radial modes with periods ranging from about 1.2 to 74 days.[14] Recent stellar evolution models suggest the pulsations are powered by the nuclear reactions in a hydrogen-burning shell that is at least partially non-convective. The star may also be fusing helium in its core.[10]

Due to their closeness to each other, little is known about the individual intrinsic properties of the members of the Rigel Ba, Bb, C triple system. All three seem to be near equally hot B-type main-sequence stars that are 3 to 4 times as massive as the Sun.[7]

Etymology and cultural significance

In the constellation of Orion, Rigel represents Orion's knee or (as its name suggests) his foot; with the nearby star Beta Eridani marking Orion's footstool.[23] Rigel is presumably the star known as "Aurvandil's toe" in Norse mythology.[68] In the Caribbean, Rigel represented the severed leg of the folkloric figure Trois Rois, himself represented by the three stars of Orion's Belt. The leg had been severed with a cutlass by the maiden Bįhi (Sirius).[69] The Lacandon people of southern Mexico knew it as tunsel ("little woodpecker").[70]

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.[71] The indigenous Boorong people of northwestern Victoria named Rigel as Collowgullouric Warepil.[72] 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. Eridanus, the river, 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.[73] The Māori people of New Zealand named Rigel as Puanga; this was said to be a daughter of Rehua (Antares), the chief of all stars.[74] Its heliacal rising presages the appearance of Matariki (the Pleiades) in the dawn sky, marking 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, mark the start of their New Year with Rigel rather than the Pleiades.[75] Puaka is a local variant used in the South Island.[76] 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 the Genpei War; the stars were seen as facing each other off and only kept apart by Orion's Belt.[77][78][79] Rigel was also known as Gin-waki, (銀脇), "the Silver (Star) beside (Mitsu-boshi)".

In modern culture

Two ships on fire near a snow-covered island or peninsular
Rigel and escort under attack
See also: Rigel in fiction

The MS Rigel was originally a Norwegian ship, built in Copenhagen in 1924. It was requisitioned by the Germans during the World War II and sunk in 1944 while being used to transport prisoners of war.[80] Two US Navy ships have borne the name USS Rigel.

The SSM-N-6 Rigel was a cruise missile program for the US Navy that was cancelled in 1953 before reaching deployment.[81]

The Rigel Skerries are a chain of small islands in Antarctica, renamed after originally being called Utskjera. They were given their current name as Rigel was used as an astrofix.[82] Mount Rigel, elevation 1,910 m, is in Antarctica.[83]

References

  1. ^ "Define Rigel at Dictionary.com". Retrieved 6 February 2012.
  2. ^ 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.
  3. ^ 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.
  4. ^ a b c Guinan, E. F.; Eaton, J. A.; Wasatonic, R.; Stewart, H.; Engle, S. G.; McCook, G. P. (2010). "Times-Series Photometry & Spectroscopy of the Bright Blue Supergiant Rigel: Probing the Atmosphere and Interior of a SN II Progenitor". Proceedings of the International Astronomical Union. 5: 359. Bibcode:2010HiA....15..359G. doi:10.1017/S1743921310009798.
  5. ^ 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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External links

source: https://en.wikipedia.org/w/index.php?title=Rigel&diff=892217729&oldid=892216091

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