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Rigel

October 20, 2023

For other uses, see Rigel (disambiguation).

Rigel is a blue supergiant star in the constellation of Orion. It has the Bayer designation β Orionis, which is Latinized to Beta Orionis and abbreviated Beta Ori or β Ori. Rigel is the brightest and most massive component – and the eponym – of a star system of at least four stars that appear as a single blue-white point of light to the naked eye. This system is located at a distance of approximately 860 light-years (260 pc) from the Sun.

Rigel
Location of Rigel (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Orion
Pronunciation /ˈraɪdʒəl/[1] or /-ɡəl/[2]
A
Right ascension 05h 14m 32.27210s[3]
Declination −08° 12′ 05.8981″[3]
Apparent magnitude (V) 0.13[4] (0.05–0.18[5])
BC
Right ascension 05h 14m 32.049s[6]
Declination −08° 12′ 14.78″[6]
Apparent magnitude (V) 6.67[7] (7.5/7.6[8])
Characteristics
A
Evolutionary stage Blue supergiant
Spectral type B8 Ia[9]
U−B color index −0.66[10]
B−V color index −0.03[10]
Variable type Alpha Cygni[11]
BC
Evolutionary stage Main sequence
Spectral type B9V + B9V[12]
Astrometry
Radial velocity (Rv)17.8±0.4[13] km/s
Proper motion (μ) RA: +1.31[3] mas/yr
Dec.: +0.50[3] mas/yr
Parallax (π)3.2352 ± 0.0553 mas[14]
Distance863[15][16] ly
(264 pc)
Absolute magnitude (MV)−7.84[9]
Orbit[12]
PrimaryA
CompanionBC
Period (P)24,000 yr
Orbit[7]
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[12]
PrimaryB
CompanionC
Period (P)63 yr
Details
A
Mass21±3[17] M☉
Radius78.9±7.4[18] R☉
Luminosity (bolometric)1.20+0.25
−0.21×105[18] L☉
Surface gravity (log g)1.75±0.10[19] cgs
Temperature12,100±150[19] K
Metallicity [Fe/H]−0.06±0.10[9] dex
Rotational velocity (v sin i)25±3[19] km/s
Age8±1[9] Myr
Ba
Mass3.84[12] M☉
Bb
Mass2.94[12] M☉
C
Mass3.84[12] M☉
Other designations
β Orionis, ADS 3823, STF 668, BU 555,[8] H II 33,[20] CCDM J05145-0812, WDS J05145-0812[21]
A: Rigel, Algebar, Elgebar, 19 Orionis, HD 34085, HR 1713, HIP 24436, SAO 131907, BD−08°1063, FK5 194
B: Rigel B, GCRV 3111
Database references
SIMBADRigel
Rigel B

A star of spectral type B8Ia, Rigel is calculated to be anywhere from 61,500 to 363,000 times as luminous as the Sun, and 18 to 24 times as massive, depending on the method and assumptions used. Its radius is more than seventy times that of the Sun, and its surface temperature is 12,100 K. Due to its stellar wind, Rigel's mass-loss is estimated to be ten million times that of the Sun. With an estimated age of seven to nine million years, Rigel has exhausted its core hydrogen fuel, expanded, and cooled to become a supergiant. It is expected to end its life as a type II supernova, leaving a neutron star or a black hole as a final remnant, depending on the initial mass of the star.

Rigel varies slightly in brightness, its apparent magnitude ranging from 0.05 to 0.18. It is classified as an Alpha Cygni variable due to the amplitude and periodicity of its brightness variation, as well as its spectral type. Its intrinsic variability is caused by pulsations in its unstable atmosphere. Rigel is generally the seventh-brightest star in the night sky and the brightest star in Orion, though it is occasionally outshone by Betelgeuse, which varies over a larger range.

A triple-star system is separated from Rigel by an angle of 9.5 arc seconds. It has an apparent magnitude of 6.7, making it 1/400th as bright as Rigel. Two stars in the system can be seen by large telescopes, and the brighter of the two is a spectroscopic binary. These three stars are all blue-white main-sequence stars, each three to four times as massive as the Sun. Rigel and the triple system orbit a common center of gravity with a period estimated to be 24,000 years. The inner stars of the triple system orbit each other every 10 days, and the outer star orbits the inner pair every 63 years. A much fainter star, separated from Rigel and the others by nearly an arc minute, may be part of the same star system.

Nomenclature Edit

 
Orion, with Rigel at bottom right, at optical wavelengths plus the Hα (hydrogen-alpha) spectral line to emphasize gas clouds

In 2016, the International Astronomical Union (IAU) included the name "Rigel" in the IAU Catalog of Star Names.[22][23] According to the IAU, this proper name applies only to the primary component A of the Rigel system. In historical astronomical catalogs, the system is listed variously as H II 33, Σ 668, β 555, or ADS 3823. For simplicity, Rigel's companions are referred to as Rigel B,[23] C, and D;[24][25] the IAU describes such names as "useful nicknames" that are "unofficial".[23] In modern comprehensive catalogs, the whole multiple star system is known as WDS 05145-0812 or CCDM 05145–0812.[8][26]

The designation of Rigel as β Orionis (Latinized to Beta Orionis) was made by Johann Bayer in 1603. The "beta" designation is commonly given to the second-brightest star in each constellation, but Rigel is almost always brighter than α Orionis (Betelgeuse).[27] 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] Bayer did not strictly order the stars by brightness, instead grouping them by magnitude.[28] Rigel and Betelgeuse were both considered to be of the first magnitude class, and in Orion the stars of each class are thought to have been ordered north to south.[29] Rigel is included in the General Catalogue of Variable Stars, but since it already has a Bayer designation it has no separate variable star designation.[30]

Rigel has many other stellar designations taken from various catalogs, 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 frequently appear in the scientific literature,[12][17][31] but rarely in popular writing.[25][32]

Observation Edit

 
Rigel A and Rigel B as they appear in a small telescope

Rigel is an intrinsic variable star with an apparent magnitude ranging from 0.05 to 0.18.[5] It is typically the seventh-brightest star in the celestial sphere, excluding the Sun, although occasionally fainter than Betelgeuse.[32] It is fainter than Capella, which may also vary slightly in brightness.[33] Rigel appears slightly blue-white and has a B-V color index of −0.06.[34] It contrasts strongly with reddish Betelgeuse.[35]

Culminating every year at midnight on 12 December, and at 9:00 pm on 24 January, Rigel is visible on winter evenings in the Northern Hemisphere and on summer evenings in the Southern Hemisphere.[27] In the Southern Hemisphere, Rigel is the first bright star of Orion visible as the constellation rises.[36] Correspondingly it is also the first star of Orion to set in most of the Northern Hemisphere. 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 north of the 82nd parallel north).[37]

Spectroscopy Edit

Rigel's spectral type is a defining point of the classification sequence for supergiants.[38][39] The overall spectrum is typical for a late B class star, with strong absorption lines of the hydrogen Balmer series as well as neutral helium lines and some of heavier elements such as oxygen, calcium, and magnesium.[40] 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.[41] Variations in the spectrum have resulted in the assignment of different classes to Rigel, such as B8 Ia, B8 Iab, and B8 Iae.[17][42]

As early as 1888, the heliocentric radial velocity of Rigel, as estimated from the Doppler shifts of its spectral lines, was seen to vary. This was confirmed and interpreted at the time as being due to a spectroscopic companion with a period of about 22 days.[43] The radial velocity has since been measured to vary by about 10 km/s around a mean of 21.5 km/s.[44]

In 1933, the Hα line in Rigel's spectrum 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.[45] 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 a dense wind close to the star and absorption from circumstellar material expanding away from the star.[45]

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.[44] 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.[46]

Variability Edit

 
A light curve for Rigel, adapted from Moravveji et al. (2012)[18]

Rigel has been known to vary in brightness since at least 1930. The small amplitude of Rigel's brightness variation requires photoelectric or CCD photometry to be reliably detected. This brightness 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 color index varies slightly, but this is not significantly correlated with its brightness variations.[47]

From analysis of Hipparcos satellite photometry, Rigel is identified as belonging to the Alpha Cygni class of variable stars,[48] defined as "non-radially pulsating supergiants of the Bep–AepIa spectral types".[33] In those spectral types, the 'e' indicates that it displays emission lines in its spectrum, while the 'p' means it has an unspecified spectral peculiarity. Alpha Cygni type variables are generally considered to be irregular[49] or have quasi-periods.[50] Rigel was added to the General Catalogue of Variable Stars in the 74th name-list of variable stars on the basis of the Hipparcos photometry,[51] which showed variations with a photographic amplitude of 0.039 magnitudes and a possible period of 2.075 days.[52] Rigel was observed with the Canadian MOST satellite for nearly 28 days in 2009. Milli-magnitude variations were observed, and gradual changes in flux suggest the presence of long-period pulsation modes.[18]

Mass loss Edit

From observations of the variable Hα spectral line, Rigel's mass-loss rate due to stellar wind is estimated be (1.5±0.4)×10−7 solar masses per year (M☉/yr)—about ten million times more than the mass-loss rate from the Sun.[53] 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 Rigel's 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.[54] It is estimated that Rigel has lost about three solar masses (M☉) since beginning life as a star of 24±3 M☉ seven to nine million years ago.[9]

Distance Edit

 
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 somewhat uncertain, different estimates being obtained by different methods. The 2007 Hipparcos new reduction of Rigel's parallax is 3.78±0.34 mas, giving a distance of 863 light-years (265 parsecs) with a margin of error of about 9%.[3] Rigel B, usually considered to be physically associated with Rigel and at the same distance, has a Gaia Data Release 3 parallax of 3.2352±0.0553 mas, suggesting a distance around 1,000 light-years (310 parsecs). However, the measurements for this object may be unreliable.[14]

Indirect distance estimation methods have also been employed. For example, Rigel is believed to be in a region of nebulosity, its radiation illuminating several nearby clouds. Most notable of these is the 5°-long IC 2118 (Witch Head Nebula),[55][56] located at an angular separation of 2.5° from the star,[55] or a projected distance of 39 light-years (12 parsecs) away.[24] From measures of other nebula-embedded stars, IC 2118's distance is estimated to be 949 ± 7 light-years (291 ± 2 parsecs).[57]

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).[31][58] 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.[42]

Stellar system Edit

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[12]

The star system of which Rigel is a part has at least four components. Rigel (sometimes called Rigel A to distinguish from the other components) has a visual companion, which is likely a close triple-star system. A fainter star at a wider separation might be a fifth component of the Rigel system.

William Herschel discovered Rigel to be a visual double star on 1 October 1781, cataloguing it as star 33 in the "second class of double stars" in his Catalogue of Double Stars,[20] usually abbreviated to H II 33, or as H 2 33 in the Washington Double Star Catalogue.[8] Friedrich Georg Wilhelm von Struve first measured the relative position of the companion in 1822, cataloguing the visual pair as Σ 668.[59][60] The secondary star is often referred to as Rigel B or β Orionis B. The angular separation of Rigel B from Rigel A is 9.5 arc seconds to its south along position angle 204°.[8][61] Although not particularly faint at visual magnitude 6.7, the overall difference in brightness from Rigel A (about 6.6 magnitudes or 440 times fainter) makes it a challenging target for telescope apertures smaller than 15 cm (6 in).[7]

At Rigel's estimated distance, Rigel B's projected separation from Rigel A is over 2,200 astronomical units (AU). Since its discovery, there has been no sign of orbital motion, although both stars share a similar common proper motion.[56][62] The pair would have an estimated orbital period of 24,000 years.[12] 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.[63]

In 1871, Sherburne Wesley Burnham suspected Rigel B to be a binary system, and in 1878, he resolved it into two components.[64] 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″.[8][64] In 2009, speckle interferometry showed the two almost identical components separated by 0.124″,[65] with visual magnitudes of 7.5 and 7.6, respectively.[8] Their estimated orbital period is 63 years.[12] Burnham listed the Rigel multiple system as β 555 in his double star catalog[64] or BU 555 in modern use.[8]

Component B is a double-lined spectroscopic binary system, which shows two sets of spectral lines combined within its single stellar spectrum. Periodic changes observed in relative positions of these lines indicate an orbital period of 9.86 days. The two spectroscopic components Rigel Ba and Rigel Bb cannot be resolved in optical telescopes but are known to both be hot stars of spectral type around B9. This spectroscopic binary, together with the close visual component Rigel C, is likely a physical triple-star system,[62] although Rigel C cannot be detected in the spectrum, which is inconsistent with its observed brightness.[7]

In 1878, Burnham found another possibly associated star of approximately 13th magnitude. He listed it as component D of β 555,[64] although it is unclear whether it is physically related or a coincidental alignment. Its 2017 separation from Rigel was 44.5″, almost due north at a position angle of 1°.[8] Gaia DR2 finds it to be a 12th magnitude sunlike star at approximately the same distance as Rigel.[66] Likely a K-type main-sequence star, 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 the star does not exist and that observed pulsations are intrinsic to Rigel itself.[62]

Physical characteristics Edit

 
Rigel's place at top-center on the Hertzsprung–Russell diagram

Rigel is a blue supergiant that has exhausted the hydrogen fuel in its core, expanded and cooled as it moved away from the main sequence across the upper part of the Hertzsprung–Russell diagram.[5][67] When it was on the main sequence, its effective temperature would have been around 30,000 K.[68] Rigel's complex variability at visual wavelengths is caused by stellar pulsations similar to those of Deneb. Further observations of radial velocity variations indicate that it simultaneously oscillates in at least 19 non-radial modes with periods ranging from about 1.2 to 74 days.[18]

Estimation of many physical characteristics of blue supergiant stars, including Rigel, is challenging due to their rarity and uncertainty about how far they are from the Sun. As such, their characteristics are mainly estimated from theoretical stellar evolution models.[69] Its effective temperature can be estimated from the spectral type and color to be around 12,100 K.[19] A mass of 21±3 M☉ at an age of 8±1 million years has been estimated by comparing evolutionary tracks, while atmospheric modeling from the spectrum gives a mass of 24±8 M☉.[9]

Although Rigel is often considered the most luminous star within 1,000 light-years of the Sun,[27][32] its energy output is poorly known. 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 (L☉),[18] but another recently published distance of 1,170 ± 130 light-years (360 ± 40 parsecs) suggests an even higher luminosity of 219,000 L☉.[9] Other calculations based on theoretical stellar evolutionary models of Rigel's atmosphere give luminosities anywhere between 83,000 L☉ and 363,000 L☉,[31] while summing the spectral energy distribution from historical photometry with the Hipparcos distance suggests a luminosity as low as 61,515±11,486 L☉.[70] 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☉.[70] An older measurement of the angular diameter gives 2.75±0.01 mas,[71] equivalent to a radius of 78.9 R☉ at 264 pc.[18] These radii are calculated assuming the Hipparcos distance of 264 pc; adopting a distance of 360 pc leads to a significantly larger size.[54]

Due to their closeness to each other and ambiguity of the spectrum, little is known about the intrinsic properties of the members of the Rigel BC triple system. All three stars seem to be near equally hot B-type main-sequence stars that are three to four times as massive as the Sun.[12]

Evolution Edit

Stellar evolution models suggest the pulsations of Rigel are powered by nuclear reactions in a hydrogen-burning shell that is at least partially non-convective. These pulsations are stronger and more numerous in stars that have evolved through a red supergiant phase and then increased in temperature to again become a blue supergiant. This is due to the decreased mass and increased levels of fusion products at the surface of the star.[68]

Rigel is likely to be fusing helium in its core.[11] Due to strong convection of helium produced in the core while Rigel was on the main sequence and in the hydrogen-burning shell since it became a supergiant, the fraction of helium at the surface has increased from 26.6% when the star formed to 32% now. The surface abundances of carbon, nitrogen, and oxygen seen in the spectrum are compatible with a post-red supergiant star only if its internal convection zones are modeled using non-homogeneous chemical conditions known as the Ledoux Criteria.[68]

Rigel is expected to eventually end its stellar life as a type II supernova.[11] It is one of the closest known potential supernova progenitors to Earth,[18] and would be expected to have a maximum apparent magnitude of around −11 (about the same brightness as a quarter Moon or around 300 times brighter than Venus ever gets.)[5] The supernova would leave behind either a black hole or a neutron star.[11]

Etymology and cultural significance Edit

 
Orion illustrated in a copy of Abd al-Rahman al-Sufi's Book of Fixed Stars. The foot on the left is annotated rijl al-jauza al-yusra, the Arabic name from which Rigel is derived.[a]

The earliest known recording of the 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"),[73] which can be traced to the 10th century.[74] "Jauzah" was a proper name for Orion; an alternative Arabic name was رجل الجبار rijl al-jabbār, "the foot of the great one", from which stems 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. [b][75] 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.[73]

With the constellation representing the mythological Greek huntsman Orion, Rigel is his knee or (as its name suggests) foot; with the nearby star Beta Eridani marking Orion's footstool.[27] Rigel is presumably the star known as "Aurvandil's toe" in Norse mythology.[76] 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).[77] The Lacandon people of southern Mexico knew it as tunsel ("little woodpecker").[78]

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.[79] The indigenous Boorong people of northwestern Victoria named Rigel as Collowgullouric Warepil.[80] 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.[81]

The Māori people of New Zealand named Rigel as Puanga, said to be a daughter of Rehua (Antares), the chief of all-stars.[82] 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.[83] Puaka is a southern name variant used in the South Island.[84]

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 off against each other and kept apart only by the three stars of Orion's Belt.[85][86][87]

In modern culture Edit

The MS Rigel was originally a Norwegian ship, built in Copenhagen in 1924. It was requisitioned by the Germans during World War II and sunk in 1944 while being used to transport prisoners of war.[88] Two US Navy ships have borne the name USS Rigel.[89][90][91] The SSM-N-6 Rigel was a cruise missile program for the US Navy that was cancelled in 1953 before reaching deployment.[92]

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.[93] Mount Rigel, elevation 1,910 m (6,270 ft), is also in Antarctica.[94]

Due to its brightness and its recognizable name, Rigel is also a popular fixture in science fiction. Fictional depictions of Rigel can be found in Star Trek, The Hitchhiker's Guide to the Galaxy, The Simpsons and many more books, films, and games.

See also Edit

Notes Edit

  1. ^ Al-Sufi's book was translated into Latin and other European languages. Al-Sufi himself planned the figures, two for each constellation: one shows how they appear to an observer looking up toward the heavens; the other how they appear to the observer looking down upon a celestial globe.[72]
  2. ^ lit."... and it is called Algebar. It is also named Rigel."

References Edit

  1. ^ Kunitzsch, Paul; Smart, Tim (2006). A Dictionary of Modern star Names: A Short Guide to 254 Star Names and Their Derivations (2nd rev. ed.). Cambridge, Massachusetts: Sky Pub. ISBN 978-1-931559-44-7.
  2. ^ Upton, Clive; Kretzschmar, William A. Jr. (2017). The Routledge Dictionary of Pronunciation for Current English (2nd ed.). Routledge. p. 1150. ISBN 978-1-138-12566-7.
  3. ^ a b c d e van Leeuwen, F. (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. S2CID 18759600.
  4. ^ Ducati, J. R. (2002). "VizieR On-line Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
  5. ^ a b c d 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.
  6. ^ a b Epchtein, N.; et al. (March 1997). "The deep near-infrared southern sky survey (DENIS)". The Messenger. 87: 27–34. Bibcode:1997Msngr..87...27E.
  7. ^ a b c d Sanford, Roscoe F. (1942). "The Spectrographic Orbit of the Companion to Rigel". The Astrophysical Journal. 95: 421. Bibcode:1942ApJ....95..421S. doi:10.1086/144412.
  8. ^ a b c d e f g h i Mason, Brian D.; Wycoff, Gary L.; Hartkopf, William I.; Douglass, Geoffrey G.; Worley, Charles E. (2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal. 122 (6): 3466–3471. Bibcode:2001AJ....122.3466M. doi:10.1086/323920. from the original on 14 March 2016. Retrieved 13 March 2016.
  9. ^ a b c d e f g Przybilla, N.; Butler, K.; Becker, S. R.; Kudritzki, R. P. (2006). "Quantitative spectroscopy of BA-type supergiants". Astronomy and Astrophysics. 445 (3): 1099–1126. arXiv:astro-ph/0509669. Bibcode:2006A&A...445.1099P. doi:10.1051/0004-6361:20053832. S2CID 118953817.
  10. ^ a b Nicolet, B. (1978). "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System". Astronomy and Astrophysics Supplement Series. 34: 1–49. Bibcode:1978A&AS...34....1N.
  11. ^ a b c d Moravveji, Ehsan; Moya, Andres; Guinan, Edward F. (2012). "Asteroseismology of the nearby SN-II Progenitor: Rigel. Part II. ε-mechanism Triggering Gravity-mode Pulsations?". The Astrophysical Journal. 749 (1): 74–84. arXiv:1202.1836. Bibcode:2012ApJ...749...74M. doi:10.1088/0004-637X/749/1/74. S2CID 119072203.
  12. ^ a b c d e f g h i j k Tokovinin, A. A. (1997). "MSC – a catalogue of physical multiple stars". Astronomy & Astrophysics Supplement Series. 124: 75–84. Bibcode:1997A&AS..124...75T. doi:10.1051/aas:1997181. S2CID 30387824.
  13. ^ Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv:1606.08053. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. S2CID 119231169.
  14. ^ a b Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  15. ^ Sessions, Larry (21 January 2020). "Rigel In Orion Is Blue-White". EarthSky. EarthSky Communications, Inc. Retrieved 15 September 2021.
  16. ^ "Rigel". Star Facts: A guide to the night sky. StarFacts.com. 17 September 2019. Retrieved 15 September 2021.
  17. ^ a b c Shultz, M.; Wade, G. A.; Petit, V.; Grunhut, J.; Neiner, C.; Hanes, D.; MiMeS Collaboration (2014). "An observational evaluation of magnetic confinement in the winds of BA supergiants". Monthly Notices of the Royal Astronomical Society. 438 (2): 1114. arXiv:1311.5116. Bibcode:2014MNRAS.438.1114S. doi:10.1093/mnras/stt2260. S2CID 118557626.
  18. ^ a b c d e f g h Moravveji, Ehsan; Guinan, Edward F.; Shultz, Matt; Williamson, Michael H.; Moya, Andres (2012). "Asteroseismology of the nearby SN-II Progenitor: Rigel. Part I. The MOST High-precision Photometry and Radial Velocity Monitoring". The Astrophysical Journal. 747 (1): 108–115. arXiv:1201.0843. Bibcode:2012ApJ...747..108M. doi:10.1088/0004-637X/747/2/108. S2CID 425831.
  19. ^ a b c d Przybilla, N. (2010). "Mixing of CNO-cycled matter in massive stars". Astronomy and Astrophysics. 517: A38. arXiv:1005.2278. Bibcode:2010A&A...517A..38P. doi:10.1051/0004-6361/201014164. S2CID 55532189.
  20. ^ a b Herschel, Mr.; Watson, Dr. (1 January 1782). "Catalogue of Double Stars. By Mr. Herschel, F. R. S. Communicated by Dr. Watson, Jun". Philosophical Transactions of the Royal Society of London. 72: 112–162 [128]. Bibcode:1782RSPT...72..112H. doi:10.1098/rstl.1782.0014. S2CID 186209247. (PDF) from the original on 3 May 2019. Retrieved 23 January 2020. Read January 10, 1782
  21. ^ "bet Ori". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 13 February 2019.
  22. ^ "IAU Catalog of Star Names". International Astronomical Union (IAU). from the original on 7 July 2018. Retrieved 28 July 2016.
  23. ^ a b c Mamajek, Eric E.; et al. (2018). "Division C: Working Group on Star Names". In Benvenuti, Piero (ed.). Transactions IAU:Volume XXXA: Reports on Astronomy 2015–2018 (PDF). Cambridge, UK: Cambridge University Press. (PDF) from the original on 23 August 2019.
  24. ^ a b c d Kaler, James B. (26 September 2009). "Rigel". Stars. from the original on 22 April 2019. Retrieved 1 February 2019.
  25. ^ a b Garfinkle, Robert A. (1997). Star-hopping: your Visa to Viewing the Universe. Cambridge, United Kingdom: Cambridge University Press. pp. 70–71. ISBN 978-0-521-59889-7.
  26. ^ Dommanget, J.; Nys, O. (1994). "Catalogue des composantes d'etoiles doubles et multiples (CCDM) premiere edition – Catalogue of the components of double and multiple stars (CCDM) first edition". Communications de l'Observatoire Royal de Belgique. 115: 1. Bibcode:1994CoORB.115....1D.
  27. ^ a b c d Schaaf, Fred (2008). The Brightest Stars: Discovering the Universe through the Sky's Most Brilliant Stars. Hoboken, New Jersey: Wiley. pp. 159–162, 257. Bibcode:2008bsdu.book.....S. ISBN 978-0-470-24917-8.
  28. ^ Ridpath, Ian (1989). "Bayer's Uranometria and Bayer letters". Star Tales. Cambridge, United Kingdom: Lutterworth Press. ISBN 978-0-7188-2695-6.
  29. ^ Moore, Patrick (1996). Brilliant Stars. London: Cassell. ISBN 978-0-304-34903-6.
  30. ^ "Nomenclature of Variable Stars". British Astronomical Association. from the original on 30 September 2016. Retrieved 11 February 2019.
  31. ^ a b c Markova, N.; Prinja, R. K.; Markov, H.; Kolka, I.; Morrison, N.; Percy, J.; Adelman, S. (2008). "Wind structure of late B supergiants. I. Multi-line analyses of near-surface and wind structure in HD 199 478 (B8 Iae)". Astronomy and Astrophysics. 487 (1): 211. arXiv:0806.0929. Bibcode:2008A&A...487..211M. doi:10.1051/0004-6361:200809376. S2CID 18067739.
  32. ^ a b c Burnham, Robert (1978) [1966]. Burnham's Celestial Handbook, Volume Two: An Observer's Guide to the Universe Beyond the Solar System. New York: Dover Publications. pp. 1299–1301. ISBN 978-0-486-23568-4.
  33. ^ a b Samus, N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2017). "General Catalogue of Variable Stars". Astronomy Reports. 5.1. 61 (1): 80–88. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. S2CID 125853869.
  34. ^ . Australia Telescope, Outreach and Education. Commonwealth Scientific and Industrial Research Organisation. 21 December 2004. Archived from the original on 18 March 2012. Retrieved 28 June 2014.
  35. ^ Universe: The Definitive Visual Guide. London: Dorling Kindersley Limited. 1 October 2012. p. 233. ISBN 978-1-4093-2825-4.
  36. ^ Ellyard, David; Tirion, Wil (2008) [1993]. The Southern Sky Guide (3rd ed.). Port Melbourne, Victoria: Cambridge University Press. pp. 58–59. ISBN 978-0-521-71405-1.
  37. ^ Kerigan, Thomas (1835). Moore's Navigation Improved: Being the Theory and Practice of Finding the Latitude, the Longitude, and the Variation of the Compass, by the Fixed Stars and Planets. To which is Prefixed, the Description and Use of the New Celestial Planisphere. London: Baldwin and Cradock. p. 132.
  38. ^ Morgan, W. W.; Abt, Helmut A.; Tapscott, J. W. (1978). Revised MK Spectral Atlas for stars earlier than the sun. Yerkes Observatory, University of Chicago. Bibcode:1978rmsa.book.....M.{{cite book}}: CS1 maint: location missing publisher (link)
  39. ^ Morgan, W. W.; Roman, Nancy G. (1950). "Revised Standards for Supergiants on the System of the Yerkes Spectral Atlas". The Astrophysical Journal. 112: 362. Bibcode:1950ApJ...112..362M. doi:10.1086/145351.
  40. ^ Abetti, Giorgio (1963). Solar research. New York: Macmillan. p. 16.
  41. ^ Morgan, William Wilson; Keenan, Philip Childs; Kellman, Edith (1943). An atlas of stellar spectra, with an outline of spectral classification. Chicago, Illinois. Bibcode:1943assw.book.....M.{{cite book}}: CS1 maint: location missing publisher (link)
  42. ^ a b Bally, J. (2008). "Overview of the Orion Complex". Handbook of Star Forming Regions: 459. arXiv:0812.0046. Bibcode:2008hsf1.book..459B.
  43. ^ Plaskett, J. S. (1909). "The spectroscopic binary beta Orionis". The Astrophysical Journal. 30: 26. Bibcode:1909ApJ....30...26P. doi:10.1086/141674.
  44. ^ a b Morrison, N. D.; Rother, R.; Kurschat, N. (2008). Hα line profile variability in the B8Ia-type supergiant Rigel (β Ori). Clumping in Hot-Star Winds. p. 155. Bibcode:2008cihw.conf..155M.
  45. ^ a b Struve, O. (1933). "An Emission Line of Hydrogen in the Spectrum of Rigel". The Astrophysical Journal. 77: 67. Bibcode:1933ApJ....77...67S. doi:10.1086/143448.
  46. ^ Israelian, G.; Chentsov, E.; Musaev, F. (1997). "The inhomogeneous circumstellar envelope of Rigel (β Orionis A)". Monthly Notices of the Royal Astronomical Society. 290 (3): 521–532. Bibcode:1997MNRAS.290..521I. doi:10.1093/mnras/290.3.521.
  47. ^ Guinan, E. F.; McCook, G. P.; Harris, W. T.; Speranzini, D.; Wacker, S. W. (1985). "Light, Color, and H-alpha Line Variations of Rigel". Information Bulletin on Variable Stars. 2762: 1. Bibcode:1985IBVS.2762....1G.
  48. ^ Waelkens, C.; Aerts, C.; Kestens, E.; Grenon, M.; Eyer, L. (1998). "Study of an unbiased sample of B stars observed with Hipparcos: the discovery of a large amount of new slowly pulsating B star". Astronomy and Astrophysics. 330: 215–221. Bibcode:1998A&A...330..215W.
  49. ^ "Variable Star Type Designations in VSX". AAVSO. from the original on 5 October 2017. Retrieved 26 April 2019.
  50. ^ Van Genderen, A. M.; Bovenschen, H.; Engelsman, E. C.; Goudfrooy, P.; Van Haarlem, M. P.; Hartmann, D.; Latour, H. J.; Ng, Y. K.; Prein, J. J.; Van Roermund, F. H. P. M.; Roogering, H. J. A.; Steeman, F. W. M.; Tijdhof, W. (1989). "Light variations of massive stars (alpha Cygni variables). IX". Astronomy and Astrophysics Supplement Series. 79: 263. Bibcode:1989A&AS...79..263V.
  51. ^ Kazarovets, E. V.; Samus, N. N.; Durlevich, O. V.; Frolov, M. S.; Antipin, S. V.; Kireeva, N. N.; Pastukhova, E. N. (1999). "The 74th Special Name-list of Variable Stars". Information Bulletin on Variable Stars. 4659: 1. Bibcode:1999IBVS.4659....1K.
  52. ^ Lefèvre, L.; Marchenko, S. V.; Moffat, A. F. J.; Acker, A. (2009). "A systematic study of variability among OB-stars based on HIPPARCOS photometry". Astronomy & Astrophysics. 507 (2): 1141–1201. Bibcode:2009A&A...507.1141L. doi:10.1051/0004-6361/200912304.
  53. ^ Chesneau, O.; Dessart, L.; Mourard, D.; Bério, Ph.; Buil, Ch.; Bonneau, D.; Borges Fernandes, M.; Clausse, J. M.; Delaa, O.; Marcotto, A.; Meilland, A.; Millour, F.; Nardetto, N.; Perraut, K.; Roussel, A.; Spang, A.; Stee, P.; Tallon-Bosc, I.; McAlister, H.; Ten Brummelaar, T.; Sturmann, J.; Sturmann, L.; Turner, N.; Farrington, C.; Goldfinger, P. J. (2010). "Time, spatial, and spectral resolution of the Hα line-formation region of Deneb and Rigel with the VEGA/CHARA interferometer". Astronomy and Astrophysics. 521: A5. arXiv:1007.2095. Bibcode:2010A&A...521A...5C. doi:10.1051/0004-6361/201014509. S2CID 10340205.
  54. ^ a b Chesneau, O.; Kaufer, A.; Stahl, O.; Colvinter, C.; Spang, A.; Dessart, L.; Prinja, R.; Chini, R. (2014). "The variable stellar wind of Rigel probed at high spatial and spectral resolution". Astronomy and Astrophysics. 566: A125. arXiv:1405.0907. Bibcode:2014A&A...566A.125C. doi:10.1051/0004-6361/201322894. S2CID 118404460.
  55. ^ a b Guieu, S.; et al. (2010). "Spitzer Observations of IC 2118". The Astrophysical Journal. 720 (1): 46–63. arXiv:1007.0241. Bibcode:2010ApJ...720...46G. doi:10.1088/0004-637X/720/1/46. S2CID 119262311.
  56. ^ a b Jedicke, Peter; Levy, David H. (1992). "Regal Rigel". The New Cosmos. Waukesha, Wisconsin: Kalmbach Books. pp. 48–53.
  57. ^ Kounkel, Marina; et al. (2018). "The APOGEE-2 Survey of the Orion Star-forming Complex. II. Six-dimensional Structure". The Astronomical Journal. 156 (3): 22. arXiv:1805.04649. Bibcode:2018AJ....156...84K. doi:10.3847/1538-3881/aad1f1. S2CID 119509277. 84.
  58. ^ Racine, R. (1968). "Stars in reflection nebulae". The Astronomical Journal. 73: 233. Bibcode:1968AJ.....73..233R. doi:10.1086/110624.
  59. ^ Struve, Friedrich Georg Wilhelm (1827). Catalogus novus stellarum duplicium et multiplicium maxima ex parte in Specula Universitatis Caesareae Dorpatensis per magnum telescopium achromaticum Fraunhoferi detectarum. Dorpati Livonorum: J.C. Schuenmann.
  60. ^ Webb, T. W. (1917). Celestial Objects for Common Telescopes. London: Longmans, Green and Co. p. 218. from the original on 4 April 2016. Retrieved 7 March 2019.
  61. ^ Bakich, Michael E. (2010). 1,001 Celestial Wonders to See Before You Die. New York: Springer. p. 434. Bibcode:2010ocws.book.....B. ISBN 978-1441917775. from the original on 1 February 2019. Retrieved 1 February 2019.
  62. ^ a b c Pourbaix, D.; et al. (2004). "SB9: The ninth catalogue of spectroscopic binary orbits". Astronomy and Astrophysics. 424 (2): 727–732. arXiv:astro-ph/0406573. Bibcode:2004A&A...424..727P. doi:10.1051/0004-6361:20041213. S2CID 119387088.
  63. ^ 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.
  64. ^ a b c d Burnham, S.W. (1900). "A General Catalogue of the Double Stars discovered by S. W. Burnham from 1871 to 1899, arranged in order of Right Ascension". Publications of the Yerkes Observatory. 1: 59–60. Bibcode:1900PYerO...1....1B.
  65. ^ Mason, Brian D.; Hartkopf, William I.; Gies, Douglas R.; Henry, Todd J.; Helsel, John W. (2009). "The High Angular Resolution Multiplicity of Massive Stars". The Astronomical Journal. 137 (2): 3358. arXiv:0811.0492. Bibcode:2009AJ....137.3358M. doi:10.1088/0004-6256/137/2/3358. S2CID 119268845.
  66. ^ 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.
  67. ^ Seeds, Michael A.; Backman, Dana (2015). Foundations of Astronomy. Boston, Massachusetts: Cengage Learning. p. 274. ISBN 978-1-305-56239-4.
  68. ^ a b c Georgy, Cyril; Saio, Hideyuki; Meynet, Georges (2014). "The puzzle of the CNO abundances of α Cygni variables resolved by the Ledoux criterion". Monthly Notices of the Royal Astronomical Society: Letters. 439: L6–L10. arXiv:1311.4744. Bibcode:2014MNRAS.439L...6G. doi:10.1093/mnrasl/slt165. S2CID 118557550.
  69. ^ Demarque, P.; Guenther, D. B.; Li, L. H.; Mazumdar, A.; Straka, C. W. (August 2008). "YREC: the Yale rotating stellar evolution code". Astrophysics and Space Science. 316 (1–4): 31–41. arXiv:0710.4003. Bibcode:2008Ap&SS.316...31D. doi:10.1007/s10509-007-9698-y. ISBN 978-1402094408. S2CID 14254892.
  70. ^ a b 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. arXiv:1712.08109. Bibcode:2018AJ....155...30B. doi:10.3847/1538-3881/aa9d8b. S2CID 119427037.
  71. ^ Aufdenberg, J. P.; et al. (2008). "Limb Darkening: Getting Warmer". In Richichi A.; Delplancke F.; Paresce F.; Chelli A. (eds.). The Power of Optical/IR Interferometry. Eso Astrophysics Symposia. Vol. 1. Berlin: Springer. pp. 71–82. Bibcode:2008poii.conf...71A. doi:10.1007/978-3-540-74256-2_8. ISBN 978-3-540-74253-1.
  72. ^ Langermann, Y. Tzvi (2018). "Mathematics, Astronomy, and Astrology". In Casagrande-Kim, Roberta; Thrope, Samuel; Ukeles, Raquel (eds.). Romance and Reason: Islamic Transformations of the Classical Past. Princeton, New Jersey: Princeton University Press. pp. 92–93. ISBN 978-0-691-18184-4.
  73. ^ a b Allen, Richard Hinckley (1963) [1899]. Star Names: Their Lore and Meaning (Reprint ed.). New York: Dover Publications Inc. pp. 312–313. ISBN 978-0-486-21079-7.
  74. ^ Kunitzsch, Paul (1959). Arabische Sternnamen in Europa (in German). Wiesbaden: Otto Harrassowitz. p. 46.
  75. ^ Kunitzsch, P. (1986). "The Star Catalogue Commonly Appended to the Alfonsine Tables". Journal for the History of Astronomy. 17 (2): 89–98. Bibcode:1986JHA....17...89K. doi:10.1177/002182868601700202. S2CID 118597258.
  76. ^ Cleasby, Richard; Vigfusson, Gudbrand (1874). An Icelandic-English Dictionary. Oxford, United Kingdom: Clarendon Press.
  77. ^ Taylor, Douglas (1946). "Notes on the Star Lore of the Caribbees". American Anthropologist. 48 (2): 215–222. doi:10.1525/aa.1946.48.2.02a00030. JSTOR 663691.
  78. ^ Milbrath, Susan (1999). Star Gods of the Maya: Astronomy in Art, Folklore, and Calendars. Austin, Texas: University of Texas Press. p. 39. ISBN 978-0-292-75226-9.
  79. ^ 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.
  80. ^ 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): 220–234. arXiv:1010.4610. Bibcode:2010JAHH...13..220H. doi:10.3724/SP.J.1440-2807.2010.03.06. S2CID 118454721.
  81. ^ Harney, Bill Yidumduma; Cairns, Hugh C. (2004) [2003]. Dark Sparklers (Revised ed.). Merimbula, New South Wales: Hugh C. Cairns. pp. 139–140. ISBN 978-0-9750908-0-0.
  82. ^ Parker, Janet; Mills, Alice; Stanton, Julie (2007). Mythology: Myths, Legends and Fantasies. New York: Struik Publishers. p. 419. ISBN 978-1-77007-453-8. from the original on 2 January 2014. Retrieved 3 November 2016.
  83. ^ Kelley, David H.; Milone, Eugene F. (2011). Exploring Ancient Skies: A Survey of Ancient and Cultural Astronomy. New York: Springer. p. 341. ISBN 978-1-4419-7623-9.
  84. ^ Best, Elsdon (1922). Astronomical Knowledge of the Maori: Genuine and Empirical. Wellington, New Zealand: Dominion Museum. pp. 39–40. from the original on 4 November 2012. Retrieved 16 November 2012.
  85. ^ Renshaw, Steve; Ihara, Saori (October 1999). "Yowatashi Boshi; Stars that Pass in the Night". Renshaw Works. Retrieved 16 June 2020.
  86. ^ "Akira Matsumura (1988). 大辞林 [Daijirin] (in Japanese). Tokyo: Sanseidō. ISBN 978-4-385-14001-8.
  87. ^ Nojiri, Hōei (2002). Shin seiza jyunrei. Tokyo: Chuokoron-Shinsha. p. 19. ISBN 978-4-12-204128-8.
  88. ^ "MS. Rigel". Minnehallen (The Memorial Hall) (in Norwegian). from the original on 4 February 2019. Retrieved 5 January 2019.
  89. ^ Silverstone, Paul H. (1968). U.S. Warships of World War II. Garden City, New York: Doubleday & Company. p. 283.
  90. ^ "NH 1874 USS RIGEL (AD-13), 1922-46". Naval History and Heritage Command. Retrieved 14 June 2020.
  91. ^ "80-G-1017252 USS Rigel (AF-58)". Naval History and Heritage Command. Retrieved 14 June 2020.
  92. ^ Yenne, Bill (2018). The Complete History of U.S. Cruise Missiles. Forest Lake, Minnesota: Specialty Press. p. 69. ISBN 978-1-58007-256-4.
  93. ^ "Antarctica Detail: ID 12640". U.S. Geological Survey. U.S. Department of the Interior. from the original on 2 February 2019. Retrieved 2 February 2019.
  94. ^ "Antarctica Detail: ID 12639". U.S. Geological Survey. U.S. Department of the Interior. Retrieved 2 February 2019.

External links Edit

 
Wikimedia Commons has media related to Rigel.
  • NASA Astronomy Picture of the Day: Rigel and the Witch Head Nebula (15 January 2018)
  • NASA Astronomy Picture of the Day: A Blazing Fireball between the Orion Nebula and Rigel (16 November 2015)
  • December double star of the month – beta Orionis Astronomical Society of Southern Africa
  • My Favorite Double Star AAVSO


October 20, 2023
rigel, other, uses, disambiguation, blue, supergiant, star, constellation, orion, bayer, designation, orionis, which, latinized, beta, orionis, abbreviated, beta, brightest, most, massive, component, eponym, star, system, least, four, stars, that, appear, sing. For other uses see Rigel disambiguation Rigel is a blue supergiant star in the constellation of Orion It has the Bayer designation b Orionis which is Latinized to Beta Orionis and abbreviated Beta Ori or b Ori Rigel is the brightest and most massive component and the eponym of a star system of at least four stars that appear as a single blue white point of light to the naked eye This system is located at a distance of approximately 860 light years 260 pc from the Sun RigelLocation of Rigel circled Observation dataEpoch J2000 0 Equinox J2000 0Constellation OrionPronunciation ˈ r aɪ dʒ el 1 or ɡ el 2 ARight ascension 05h 14m 32 27210s 3 Declination 08 12 05 8981 3 Apparent magnitude V 0 13 4 0 05 0 18 5 BCRight ascension 05h 14m 32 049s 6 Declination 08 12 14 78 6 Apparent magnitude V 6 67 7 7 5 7 6 8 CharacteristicsAEvolutionary stage Blue supergiantSpectral type B8 Ia 9 U B color index 0 66 10 B V color index 0 03 10 Variable type Alpha Cygni 11 BCEvolutionary stage Main sequenceSpectral type B9V B9V 12 AstrometryRadial velocity Rv 17 8 0 4 13 km sProper motion m RA 1 31 3 mas yr Dec 0 50 3 mas yrParallax p 3 2352 0 0553 mas 14 Distance863 15 16 ly 264 pc Absolute magnitude MV 7 84 9 Orbit 12 PrimaryACompanionBCPeriod P 24 000 yrOrbit 7 PrimaryBaCompanionBbPeriod P 9 860 daysEccentricity e 0 1Semi amplitude K1 primary 25 0 km sSemi amplitude K2 secondary 32 6 km sOrbit 12 PrimaryBCompanionCPeriod P 63 yrDetailsAMass21 3 17 M Radius78 9 7 4 18 R Luminosity bolometric 1 20 0 25 0 21 105 18 L Surface gravity log g 1 75 0 10 19 cgsTemperature12 100 150 19 KMetallicity Fe H 0 06 0 10 9 dexRotational velocity v sin i 25 3 19 km sAge8 1 9 MyrBaMass3 84 12 M BbMass2 94 12 M CMass3 84 12 M Other designationsb Orionis ADS 3823 STF 668 BU 555 8 H II 33 20 CCDM J05145 0812 WDS J05145 0812 21 A Rigel Algebar Elgebar 19 Orionis HD 34085 HR 1713 HIP 24436 SAO 131907 BD 08 1063 FK5 194B Rigel B GCRV 3111Database referencesSIMBADRigelRigel BA star of spectral type B8Ia Rigel is calculated to be anywhere from 61 500 to 363 000 times as luminous as the Sun and 18 to 24 times as massive depending on the method and assumptions used Its radius is more than seventy times that of the Sun and its surface temperature is 12 100 K Due to its stellar wind Rigel s mass loss is estimated to be ten million times that of the Sun With an estimated age of seven to nine million years Rigel has exhausted its core hydrogen fuel expanded and cooled to become a supergiant It is expected to end its life as a type II supernova leaving a neutron star or a black hole as a final remnant depending on the initial mass of the star Rigel varies slightly in brightness its apparent magnitude ranging from 0 05 to 0 18 It is classified as an Alpha Cygni variable due to the amplitude and periodicity of its brightness variation as well as its spectral type Its intrinsic variability is caused by pulsations in its unstable atmosphere Rigel is generally the seventh brightest star in the night sky and the brightest star in Orion though it is occasionally outshone by Betelgeuse which varies over a larger range A triple star system is separated from Rigel by an angle of 9 5 arc seconds It has an apparent magnitude of 6 7 making it 1 400th as bright as Rigel Two stars in the system can be seen by large telescopes and the brighter of the two is a spectroscopic binary These three stars are all blue white main sequence stars each three to four times as massive as the Sun Rigel and the triple system orbit a common center of gravity with a period estimated to be 24 000 years The inner stars of the triple system orbit each other every 10 days and the outer star orbits the inner pair every 63 years A much fainter star separated from Rigel and the others by nearly an arc minute may be part of the same star system Contents 1 Nomenclature 2 Observation 2 1 Spectroscopy 2 2 Variability 2 3 Mass loss 3 Distance 4 Stellar system 5 Physical characteristics 6 Evolution 7 Etymology and cultural significance 8 In modern culture 9 See also 10 Notes 11 References 12 External linksNomenclature Edit nbsp Orion with Rigel at bottom right at optical wavelengths plus the Ha hydrogen alpha spectral line to emphasize gas cloudsIn 2016 the International Astronomical Union IAU included the name Rigel in the IAU Catalog of Star Names 22 23 According to the IAU this proper name applies only to the primary component A of the Rigel system In historical astronomical catalogs the system is listed variously as H II 33 S 668 b 555 or ADS 3823 For simplicity Rigel s companions are referred to as Rigel B 23 C and D 24 25 the IAU describes such names as useful nicknames that are unofficial 23 In modern comprehensive catalogs the whole multiple star system is known as WDS 05145 0812 or CCDM 05145 0812 8 26 The designation of Rigel as b Orionis Latinized to Beta Orionis was made by Johann Bayer in 1603 The beta designation is commonly given to the second brightest star in each constellation but Rigel is almost always brighter than a Orionis Betelgeuse 27 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 Bayer did not strictly order the stars by brightness instead grouping them by magnitude 28 Rigel and Betelgeuse were both considered to be of the first magnitude class and in Orion the stars of each class are thought to have been ordered north to south 29 Rigel is included in the General Catalogue of Variable Stars but since it already has a Bayer designation it has no separate variable star designation 30 Rigel has many other stellar designations taken from various catalogs 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 frequently appear in the scientific literature 12 17 31 but rarely in popular writing 25 32 Observation Edit nbsp Rigel A and Rigel B as they appear in a small telescopeRigel is an intrinsic variable star with an apparent magnitude ranging from 0 05 to 0 18 5 It is typically the seventh brightest star in the celestial sphere excluding the Sun although occasionally fainter than Betelgeuse 32 It is fainter than Capella which may also vary slightly in brightness 33 Rigel appears slightly blue white and has a B V color index of 0 06 34 It contrasts strongly with reddish Betelgeuse 35 Culminating every year at midnight on 12 December and at 9 00 pm on 24 January Rigel is visible on winter evenings in the Northern Hemisphere and on summer evenings in the Southern Hemisphere 27 In the Southern Hemisphere Rigel is the first bright star of Orion visible as the constellation rises 36 Correspondingly it is also the first star of Orion to set in most of the Northern Hemisphere 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 north of the 82nd parallel north 37 Spectroscopy Edit Rigel s spectral type is a defining point of the classification sequence for supergiants 38 39 The overall spectrum is typical for a late B class star with strong absorption lines of the hydrogen Balmer series as well as neutral helium lines and some of heavier elements such as oxygen calcium and magnesium 40 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 41 Variations in the spectrum have resulted in the assignment of different classes to Rigel such as B8 Ia B8 Iab and B8 Iae 17 42 As early as 1888 the heliocentric radial velocity of Rigel as estimated from the Doppler shifts of its spectral lines was seen to vary This was confirmed and interpreted at the time as being due to a spectroscopic companion with a period of about 22 days 43 The radial velocity has since been measured to vary by about 10 km s around a mean of 21 5 km s 44 In 1933 the Ha line in Rigel s spectrum 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 45 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 a dense wind close to the star and absorption from circumstellar material expanding away from the star 45 The unusual Ha 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 Ha line 44 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 46 Variability Edit nbsp A light curve for Rigel adapted from Moravveji et al 2012 18 Rigel has been known to vary in brightness since at least 1930 The small amplitude of Rigel s brightness variation requires photoelectric or CCD photometry to be reliably detected This brightness 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 color index varies slightly but this is not significantly correlated with its brightness variations 47 From analysis of Hipparcos satellite photometry Rigel is identified as belonging to the Alpha Cygni class of variable stars 48 defined as non radially pulsating supergiants of the Bep AepIa spectral types 33 In those spectral types the e indicates that it displays emission lines in its spectrum while the p means it has an unspecified spectral peculiarity Alpha Cygni type variables are generally considered to be irregular 49 or have quasi periods 50 Rigel was added to the General Catalogue of Variable Stars in the 74th name list of variable stars on the basis of the Hipparcos photometry 51 which showed variations with a photographic amplitude of 0 039 magnitudes and a possible period of 2 075 days 52 Rigel was observed with the Canadian MOST satellite for nearly 28 days in 2009 Milli magnitude variations were observed and gradual changes in flux suggest the presence of long period pulsation modes 18 Mass loss Edit From observations of the variable Ha spectral line Rigel s mass loss rate due to stellar wind is estimated be 1 5 0 4 10 7 solar masses per year M yr about ten million times more than the mass loss rate from the Sun 53 More detailed optical and K band infrared spectroscopic observations together with VLTI interferometry were taken from 2006 to 2010 Analysis of the Ha and Hg line profiles and measurement of the regions producing the lines show that Rigel s stellar wind varies greatly in structure and strength Loop and arm structures were also detected within the wind Calculations of mass loss from the Hg 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 Ha line give lower results around 1 5 10 7 M yr The terminal wind velocity is 300 km s 54 It is estimated that Rigel has lost about three solar masses M since beginning life as a star of 24 3 M seven to nine million years ago 9 Distance Edit nbsp 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 somewhat uncertain different estimates being obtained by different methods The 2007 Hipparcos new reduction of Rigel s parallax is 3 78 0 34 mas giving a distance of 863 light years 265 parsecs with a margin of error of about 9 3 Rigel B usually considered to be physically associated with Rigel and at the same distance has a Gaia Data Release 3 parallax of 3 2352 0 0553 mas suggesting a distance around 1 000 light years 310 parsecs However the measurements for this object may be unreliable 14 Indirect distance estimation methods have also been employed For example Rigel is believed to be in a region of nebulosity its radiation illuminating several nearby clouds Most notable of these is the 5 long IC 2118 Witch Head Nebula 55 56 located at an angular separation of 2 5 from the star 55 or a projected distance of 39 light years 12 parsecs away 24 From measures of other nebula embedded stars IC 2118 s distance is estimated to be 949 7 light years 291 2 parsecs 57 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 31 58 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 42 Stellar system EditRigelSeparation 9 5 Period 24 000 yBaSeparation 0 58 mas Period 9 860 dBbSeparation 0 1 Period 63 yCHierarchical scheme for Rigel s components 12 The star system of which Rigel is a part has at least four components Rigel sometimes called Rigel A to distinguish from the other components has a visual companion which is likely a close triple star system A fainter star at a wider separation might be a fifth component of the Rigel system William Herschel discovered Rigel to be a visual double star on 1 October 1781 cataloguing it as star 33 in the second class of double stars in his Catalogue of Double Stars 20 usually abbreviated to H II 33 or as H 2 33 in the Washington Double Star Catalogue 8 Friedrich Georg Wilhelm von Struve first measured the relative position of the companion in 1822 cataloguing the visual pair as S 668 59 60 The secondary star is often referred to as Rigel B or b Orionis B The angular separation of Rigel B from Rigel A is 9 5 arc seconds to its south along position angle 204 8 61 Although not particularly faint at visual magnitude 6 7 the overall difference in brightness from Rigel A about 6 6 magnitudes or 440 times fainter makes it a challenging target for telescope apertures smaller than 15 cm 6 in 7 At Rigel s estimated distance Rigel B s projected separation from Rigel A is over 2 200 astronomical units AU Since its discovery there has been no sign of orbital motion although both stars share a similar common proper motion 56 62 The pair would have an estimated orbital period of 24 000 years 12 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 63 In 1871 Sherburne Wesley Burnham suspected Rigel B to be a binary system and in 1878 he resolved it into two components 64 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 8 64 In 2009 speckle interferometry showed the two almost identical components separated by 0 124 65 with visual magnitudes of 7 5 and 7 6 respectively 8 Their estimated orbital period is 63 years 12 Burnham listed the Rigel multiple system as b 555 in his double star catalog 64 or BU 555 in modern use 8 Component B is a double lined spectroscopic binary system which shows two sets of spectral lines combined within its single stellar spectrum Periodic changes observed in relative positions of these lines indicate an orbital period of 9 86 days The two spectroscopic components Rigel Ba and Rigel Bb cannot be resolved in optical telescopes but are known to both be hot stars of spectral type around B9 This spectroscopic binary together with the close visual component Rigel C is likely a physical triple star system 62 although Rigel C cannot be detected in the spectrum which is inconsistent with its observed brightness 7 In 1878 Burnham found another possibly associated star of approximately 13th magnitude He listed it as component D of b 555 64 although it is unclear whether it is physically related or a coincidental alignment Its 2017 separation from Rigel was 44 5 almost due north at a position angle of 1 8 Gaia DR2 finds it to be a 12th magnitude sunlike star at approximately the same distance as Rigel 66 Likely a K type main sequence star 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 the star does not exist and that observed pulsations are intrinsic to Rigel itself 62 Physical characteristics Edit nbsp Rigel s place at top center on the Hertzsprung Russell diagramRigel is a blue supergiant that has exhausted the hydrogen fuel in its core expanded and cooled as it moved away from the main sequence across the upper part of the Hertzsprung Russell diagram 5 67 When it was on the main sequence its effective temperature would have been around 30 000 K 68 Rigel s complex variability at visual wavelengths is caused by stellar pulsations similar to those of Deneb Further observations of radial velocity variations indicate that it simultaneously oscillates in at least 19 non radial modes with periods ranging from about 1 2 to 74 days 18 Estimation of many physical characteristics of blue supergiant stars including Rigel is challenging due to their rarity and uncertainty about how far they are from the Sun As such their characteristics are mainly estimated from theoretical stellar evolution models 69 Its effective temperature can be estimated from the spectral type and color to be around 12 100 K 19 A mass of 21 3 M at an age of 8 1 million years has been estimated by comparing evolutionary tracks while atmospheric modeling from the spectrum gives a mass of 24 8 M 9 Although Rigel is often considered the most luminous star within 1 000 light years of the Sun 27 32 its energy output is poorly known 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 L 18 but another recently published distance of 1 170 130 light years 360 40 parsecs suggests an even higher luminosity of 219 000 L 9 Other calculations based on theoretical stellar evolutionary models of Rigel s atmosphere give luminosities anywhere between 83 000 L and 363 000 L 31 while summing the spectral energy distribution from historical photometry with the Hipparcos distance suggests a luminosity as low as 61 515 11 486 L 70 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 70 An older measurement of the angular diameter gives 2 75 0 01 mas 71 equivalent to a radius of 78 9 R at 264 pc 18 These radii are calculated assuming the Hipparcos distance of 264 pc adopting a distance of 360 pc leads to a significantly larger size 54 Due to their closeness to each other and ambiguity of the spectrum little is known about the intrinsic properties of the members of the Rigel BC triple system All three stars seem to be near equally hot B type main sequence stars that are three to four times as massive as the Sun 12 Evolution EditStellar evolution models suggest the pulsations of Rigel are powered by nuclear reactions in a hydrogen burning shell that is at least partially non convective These pulsations are stronger and more numerous in stars that have evolved through a red supergiant phase and then increased in temperature to again become a blue supergiant This is due to the decreased mass and increased levels of fusion products at the surface of the star 68 Rigel is likely to be fusing helium in its core 11 Due to strong convection of helium produced in the core while Rigel was on the main sequence and in the hydrogen burning shell since it became a supergiant the fraction of helium at the surface has increased from 26 6 when the star formed to 32 now The surface abundances of carbon nitrogen and oxygen seen in the spectrum are compatible with a post red supergiant star only if its internal convection zones are modeled using non homogeneous chemical conditions known as the Ledoux Criteria 68 Rigel is expected to eventually end its stellar life as a type II supernova 11 It is one of the closest known potential supernova progenitors to Earth 18 and would be expected to have a maximum apparent magnitude of around 11 about the same brightness as a quarter Moon or around 300 times brighter than Venus ever gets 5 The supernova would leave behind either a black hole or a neutron star 11 Etymology and cultural significance Edit nbsp Orion illustrated in a copy of Abd al Rahman al Sufi s Book of Fixed Stars The foot on the left is annotated rijl al jauza al yusra the Arabic name from which Rigel is derived a The earliest known recording of the name Rigel is in the Alfonsine tables of 1521 It is derived from the Arabic name Rijl Jauzah al Yusra the left leg foot of Jauzah i e rijl meaning leg foot 73 which can be traced to the 10th century 74 Jauzah was a proper name for Orion an alternative Arabic name was رجل الجبار rijl al jabbar the foot of the great one from which stems 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 b 75 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 73 With the constellation representing the mythological Greek huntsman Orion Rigel is his knee or as its name suggests foot with the nearby star Beta Eridani marking Orion s footstool 27 Rigel is presumably the star known as Aurvandil s toe in Norse mythology 76 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 77 The Lacandon people of southern Mexico knew it as tunsel little woodpecker 78 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 79 The indigenous Boorong people of northwestern Victoria named Rigel as Collowgullouric Warepil 80 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 81 The Maori people of New Zealand named Rigel as Puanga said to be a daughter of Rehua Antares the chief of all stars 82 Its heliacal rising presages the appearance of Matariki the Pleiades in the dawn sky marking the Maori 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 83 Puaka is a southern name variant used in the South Island 84 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 off against each other and kept apart only by the three stars of Orion s Belt 85 86 87 In modern culture EditThe MS Rigel was originally a Norwegian ship built in Copenhagen in 1924 It was requisitioned by the Germans during World War II and sunk in 1944 while being used to transport prisoners of war 88 Two US Navy ships have borne the name USS Rigel 89 90 91 The SSM N 6 Rigel was a cruise missile program for the US Navy that was cancelled in 1953 before reaching deployment 92 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 93 Mount Rigel elevation 1 910 m 6 270 ft is also in Antarctica 94 Due to its brightness and its recognizable name Rigel is also a popular fixture in science fiction Fictional depictions of Rigel can be found in Star Trek The Hitchhiker s Guide to the Galaxy The Simpsons and many more books films and games See also EditOrion in Chinese astronomyNotes Edit Al Sufi s book was translated into Latin and other European languages Al Sufi himself planned the figures two for each constellation one shows how they appear to an observer looking up toward the heavens the other how they appear to the observer looking down upon a celestial globe 72 lit and it is called Algebar It is also named Rigel References Edit Kunitzsch Paul Smart Tim 2006 A Dictionary of Modern star Names A Short Guide to 254 Star Names and Their Derivations 2nd rev ed Cambridge Massachusetts Sky Pub ISBN 978 1 931559 44 7 Upton Clive Kretzschmar William A Jr 2017 The Routledge Dictionary of Pronunciation for Current English 2nd ed Routledge p 1150 ISBN 978 1 138 12566 7 a b c d e van Leeuwen F 2007 Validation of the new Hipparcos reduction Astronomy and Astrophysics 474 2 653 664 arXiv 0708 1752 Bibcode 2007A amp A 474 653V doi 10 1051 0004 6361 20078357 S2CID 18759600 Ducati J R 2002 VizieR On line Data Catalog Catalogue of Stellar Photometry in Johnson s 11 color system CDS ADC Collection of Electronic Catalogues 2237 Bibcode 2002yCat 2237 0D a b c d Guinan E F Eaton J A Wasatonic R Stewart H Engle S G McCook G P 2010 Times Series Photometry amp 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 a b Epchtein N et al March 1997 The deep near infrared southern sky survey DENIS The Messenger 87 27 34 Bibcode 1997Msngr 87 27E a b c d Sanford Roscoe F 1942 The Spectrographic Orbit of the Companion to Rigel The Astrophysical Journal 95 421 Bibcode 1942ApJ 95 421S doi 10 1086 144412 a b c d e f g h i Mason Brian D Wycoff Gary L Hartkopf William I Douglass Geoffrey G Worley Charles E 2001 The 2001 US Naval Observatory Double Star CD ROM I The Washington Double Star Catalog The Astronomical Journal 122 6 3466 3471 Bibcode 2001AJ 122 3466M doi 10 1086 323920 Archived from the original on 14 March 2016 Retrieved 13 March 2016 a b c d e f g Przybilla N Butler K Becker S R Kudritzki R P 2006 Quantitative spectroscopy of BA type supergiants Astronomy and Astrophysics 445 3 1099 1126 arXiv astro ph 0509669 Bibcode 2006A amp A 445 1099P doi 10 1051 0004 6361 20053832 S2CID 118953817 a b Nicolet B 1978 Photoelectric photometric Catalogue of homogeneous measurements in the UBV System Astronomy and Astrophysics Supplement Series 34 1 49 Bibcode 1978A amp AS 34 1N a b c d Moravveji Ehsan Moya Andres Guinan Edward F 2012 Asteroseismology of the nearby SN II Progenitor Rigel Part II e mechanism Triggering Gravity mode Pulsations The Astrophysical Journal 749 1 74 84 arXiv 1202 1836 Bibcode 2012ApJ 749 74M doi 10 1088 0004 637X 749 1 74 S2CID 119072203 a b c d e f g h i j k Tokovinin A A 1997 MSC a catalogue of physical multiple stars Astronomy amp Astrophysics Supplement Series 124 75 84 Bibcode 1997A amp AS 124 75T doi 10 1051 aas 1997181 S2CID 30387824 Gontcharov G A 2006 Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system Astronomy Letters 32 11 759 771 arXiv 1606 08053 Bibcode 2006AstL 32 759G doi 10 1134 S1063773706110065 S2CID 119231169 a b Vallenari A et al Gaia collaboration 2023 Gaia Data Release 3 Summary of the content and survey properties Astronomy and Astrophysics 674 A1 arXiv 2208 00211 Bibcode 2023A amp A 674A 1G doi 10 1051 0004 6361 202243940 S2CID 244398875 Gaia DR3 record for this source at VizieR Sessions Larry 21 January 2020 Rigel In Orion Is Blue White EarthSky EarthSky Communications Inc Retrieved 15 September 2021 Rigel Star Facts A guide to the night sky StarFacts com 17 September 2019 Retrieved 15 September 2021 a b c Shultz M Wade G A Petit V Grunhut J Neiner C Hanes D MiMeS Collaboration 2014 An observational evaluation of magnetic confinement in the winds of BA supergiants Monthly Notices of the Royal Astronomical Society 438 2 1114 arXiv 1311 5116 Bibcode 2014MNRAS 438 1114S doi 10 1093 mnras stt2260 S2CID 118557626 a b c d e f g h Moravveji Ehsan Guinan Edward F Shultz Matt Williamson Michael H Moya Andres 2012 Asteroseismology of the nearby SN II Progenitor Rigel Part I The MOST High precision Photometry and Radial Velocity Monitoring The Astrophysical Journal 747 1 108 115 arXiv 1201 0843 Bibcode 2012ApJ 747 108M doi 10 1088 0004 637X 747 2 108 S2CID 425831 a b c d Przybilla N 2010 Mixing of CNO cycled matter in massive stars Astronomy and Astrophysics 517 A38 arXiv 1005 2278 Bibcode 2010A amp A 517A 38P doi 10 1051 0004 6361 201014164 S2CID 55532189 a b Herschel Mr Watson Dr 1 January 1782 Catalogue of Double Stars By Mr Herschel F R S Communicated by Dr Watson Jun Philosophical Transactions of the Royal Society of London 72 112 162 128 Bibcode 1782RSPT 72 112H doi 10 1098 rstl 1782 0014 S2CID 186209247 Archived PDF from the original on 3 May 2019 Retrieved 23 January 2020 Read January 10 1782 bet Ori SIMBAD Centre de donnees astronomiques de Strasbourg Retrieved 13 February 2019 IAU Catalog of Star Names International Astronomical Union IAU Archived from the original on 7 July 2018 Retrieved 28 July 2016 a b c Mamajek Eric E et al 2018 Division C Working Group on Star Names In Benvenuti Piero ed Transactions IAU Volume XXXA Reports on Astronomy 2015 2018 PDF Cambridge UK Cambridge University Press Archived PDF from the original on 23 August 2019 a b c d Kaler James B 26 September 2009 Rigel Stars Archived from the original on 22 April 2019 Retrieved 1 February 2019 a b Garfinkle Robert A 1997 Star hopping your Visa to Viewing the Universe Cambridge United Kingdom Cambridge University Press pp 70 71 ISBN 978 0 521 59889 7 Dommanget J Nys O 1994 Catalogue des composantes d etoiles doubles et multiples CCDM premiere edition Catalogue of the components of double and multiple stars CCDM first edition Communications de l Observatoire Royal de Belgique 115 1 Bibcode 1994CoORB 115 1D a b c d Schaaf Fred 2008 The Brightest Stars Discovering the Universe through the Sky s Most Brilliant Stars Hoboken New Jersey Wiley pp 159 162 257 Bibcode 2008bsdu book S ISBN 978 0 470 24917 8 Ridpath Ian 1989 Bayer s Uranometria and Bayer letters Star Tales Cambridge United Kingdom Lutterworth Press ISBN 978 0 7188 2695 6 Moore Patrick 1996 Brilliant Stars London Cassell ISBN 978 0 304 34903 6 Nomenclature of Variable Stars British Astronomical Association Archived from the original on 30 September 2016 Retrieved 11 February 2019 a b c Markova N Prinja R K Markov H Kolka I Morrison N Percy J Adelman S 2008 Wind structure of late B supergiants I Multi line analyses of near surface and wind structure in HD 199 478 B8 Iae Astronomy and Astrophysics 487 1 211 arXiv 0806 0929 Bibcode 2008A amp A 487 211M doi 10 1051 0004 6361 200809376 S2CID 18067739 a b c Burnham Robert 1978 1966 Burnham s Celestial Handbook Volume Two An Observer s Guide to the Universe Beyond the Solar System New York Dover Publications pp 1299 1301 ISBN 978 0 486 23568 4 a b Samus N N Kazarovets E V Durlevich O V Kireeva N N Pastukhova E N 2017 General Catalogue of Variable Stars Astronomy Reports 5 1 61 1 80 88 Bibcode 2017ARep 61 80S doi 10 1134 S1063772917010085 S2CID 125853869 The Colour of Stars Australia Telescope Outreach and Education Commonwealth Scientific and Industrial Research Organisation 21 December 2004 Archived from the original on 18 March 2012 Retrieved 28 June 2014 Universe The Definitive Visual Guide London Dorling Kindersley Limited 1 October 2012 p 233 ISBN 978 1 4093 2825 4 Ellyard David Tirion Wil 2008 1993 The Southern Sky Guide 3rd ed Port Melbourne Victoria Cambridge University Press pp 58 59 ISBN 978 0 521 71405 1 Kerigan Thomas 1835 Moore s Navigation Improved Being the Theory and Practice of Finding the Latitude the Longitude and the Variation of the Compass by the Fixed Stars and Planets To which is Prefixed the Description and Use of the New Celestial Planisphere London Baldwin and Cradock p 132 Morgan W W Abt Helmut A Tapscott J W 1978 Revised MK Spectral Atlas for stars earlier than the sun Yerkes Observatory University of Chicago Bibcode 1978rmsa book M a href Template Cite book html title Template Cite book cite book a CS1 maint location missing publisher link Morgan W W Roman Nancy G 1950 Revised Standards for Supergiants on the System of the Yerkes Spectral Atlas The Astrophysical Journal 112 362 Bibcode 1950ApJ 112 362M doi 10 1086 145351 Abetti Giorgio 1963 Solar research New York Macmillan p 16 Morgan William Wilson Keenan Philip Childs Kellman Edith 1943 An atlas of stellar spectra with an outline of spectral classification Chicago Illinois Bibcode 1943assw book M a href Template Cite book html title Template Cite book cite book a CS1 maint location missing publisher link a b Bally J 2008 Overview of the Orion Complex Handbook of Star Forming Regions 459 arXiv 0812 0046 Bibcode 2008hsf1 book 459B Plaskett J S 1909 The spectroscopic binary beta Orionis The Astrophysical Journal 30 26 Bibcode 1909ApJ 30 26P doi 10 1086 141674 a b Morrison N D Rother R Kurschat N 2008 Ha line profile variability in the B8Ia type supergiant Rigel b Ori Clumping in Hot Star Winds p 155 Bibcode 2008cihw conf 155M a b Struve O 1933 An Emission Line of Hydrogen in the Spectrum of Rigel The Astrophysical Journal 77 67 Bibcode 1933ApJ 77 67S doi 10 1086 143448 Israelian G Chentsov E Musaev F 1997 The inhomogeneous circumstellar envelope of Rigel b Orionis A Monthly Notices of the Royal Astronomical Society 290 3 521 532 Bibcode 1997MNRAS 290 521I doi 10 1093 mnras 290 3 521 Guinan E F McCook G P Harris W T Speranzini D Wacker S W 1985 Light Color and H alpha Line Variations of Rigel Information Bulletin on Variable Stars 2762 1 Bibcode 1985IBVS 2762 1G Waelkens C Aerts C Kestens E Grenon M Eyer L 1998 Study of an unbiased sample of B stars observed with Hipparcos the discovery of a large amount of new slowly pulsating B star Astronomy and Astrophysics 330 215 221 Bibcode 1998A amp A 330 215W Variable Star Type Designations in VSX AAVSO Archived from the original on 5 October 2017 Retrieved 26 April 2019 Van Genderen A M Bovenschen H Engelsman E C Goudfrooy P Van Haarlem M P Hartmann D Latour H J Ng Y K Prein J J Van Roermund F H P M Roogering H J A Steeman F W M Tijdhof W 1989 Light variations of massive stars alpha Cygni variables IX Astronomy and Astrophysics Supplement Series 79 263 Bibcode 1989A amp AS 79 263V Kazarovets E V Samus N N Durlevich O V Frolov M S Antipin S V Kireeva N N Pastukhova E N 1999 The 74th Special Name list of Variable Stars Information Bulletin on Variable Stars 4659 1 Bibcode 1999IBVS 4659 1K Lefevre L Marchenko S V Moffat A F J Acker A 2009 A systematic study of variability among OB stars based on HIPPARCOS photometry Astronomy amp Astrophysics 507 2 1141 1201 Bibcode 2009A amp A 507 1141L doi 10 1051 0004 6361 200912304 Chesneau O Dessart L Mourard D Berio Ph Buil Ch Bonneau D Borges Fernandes M Clausse J M Delaa O Marcotto A Meilland A Millour F Nardetto N Perraut K Roussel A Spang A Stee P Tallon Bosc I McAlister H Ten Brummelaar T Sturmann J Sturmann L Turner N Farrington C Goldfinger P J 2010 Time spatial and spectral resolution of the Ha line formation region of Deneb and Rigel with the VEGA CHARA interferometer Astronomy and Astrophysics 521 A5 arXiv 1007 2095 Bibcode 2010A amp A 521A 5C doi 10 1051 0004 6361 201014509 S2CID 10340205 a b Chesneau O Kaufer A Stahl O Colvinter C Spang A Dessart L Prinja R Chini R 2014 The variable stellar wind of Rigel probed at high spatial and spectral resolution Astronomy and Astrophysics 566 A125 arXiv 1405 0907 Bibcode 2014A amp A 566A 125C doi 10 1051 0004 6361 201322894 S2CID 118404460 a b Guieu S et al 2010 Spitzer Observations of IC 2118 The Astrophysical Journal 720 1 46 63 arXiv 1007 0241 Bibcode 2010ApJ 720 46G doi 10 1088 0004 637X 720 1 46 S2CID 119262311 a b Jedicke Peter Levy David H 1992 Regal Rigel The New Cosmos Waukesha Wisconsin Kalmbach Books pp 48 53 Kounkel Marina et al 2018 The APOGEE 2 Survey of the Orion Star forming Complex II Six dimensional Structure The Astronomical Journal 156 3 22 arXiv 1805 04649 Bibcode 2018AJ 156 84K doi 10 3847 1538 3881 aad1f1 S2CID 119509277 84 Racine R 1968 Stars in reflection nebulae The Astronomical Journal 73 233 Bibcode 1968AJ 73 233R doi 10 1086 110624 Struve Friedrich Georg Wilhelm 1827 Catalogus novus stellarum duplicium et multiplicium maxima ex parte in Specula Universitatis Caesareae Dorpatensis per magnum telescopium achromaticum Fraunhoferi detectarum Dorpati Livonorum J C Schuenmann Webb T W 1917 Celestial Objects for Common Telescopes London Longmans Green and Co p 218 Archived from the original on 4 April 2016 Retrieved 7 March 2019 Bakich Michael E 2010 1 001 Celestial Wonders to See Before You Die New York Springer p 434 Bibcode 2010ocws book B ISBN 978 1441917775 Archived from the original on 1 February 2019 Retrieved 1 February 2019 a b c Pourbaix D et al 2004 SB9 The ninth catalogue of spectroscopic binary orbits Astronomy and Astrophysics 424 2 727 732 arXiv astro ph 0406573 Bibcode 2004A amp A 424 727P doi 10 1051 0004 6361 20041213 S2CID 119387088 Brown A G A et al Gaia collaboration August 2018 Gaia Data Release 2 Summary of the contents and survey properties Astronomy amp Astrophysics 616 A1 arXiv 1804 09365 Bibcode 2018A amp A 616A 1G doi 10 1051 0004 6361 201833051 Gaia DR2 record for this source at VizieR a b c d Burnham S W 1900 A General Catalogue of the Double Stars discovered by S W Burnham from 1871 to 1899 arranged in order of Right Ascension Publications of the Yerkes Observatory 1 59 60 Bibcode 1900PYerO 1 1B Mason Brian D Hartkopf William I Gies Douglas R Henry Todd J Helsel John W 2009 The High Angular Resolution Multiplicity of Massive Stars The Astronomical Journal 137 2 3358 arXiv 0811 0492 Bibcode 2009AJ 137 3358M doi 10 1088 0004 6256 137 2 3358 S2CID 119268845 Brown A G A et al Gaia collaboration August 2018 Gaia Data Release 2 Summary of the contents and survey properties Astronomy amp Astrophysics 616 A1 arXiv 1804 09365 Bibcode 2018A amp A 616A 1G doi 10 1051 0004 6361 201833051 Gaia DR2 record for this source at VizieR Seeds Michael A Backman Dana 2015 Foundations of Astronomy Boston Massachusetts Cengage Learning p 274 ISBN 978 1 305 56239 4 a b c Georgy Cyril Saio Hideyuki Meynet Georges 2014 The puzzle of the CNO abundances of a Cygni variables resolved by the Ledoux criterion Monthly Notices of the Royal Astronomical Society Letters 439 L6 L10 arXiv 1311 4744 Bibcode 2014MNRAS 439L 6G doi 10 1093 mnrasl slt165 S2CID 118557550 Demarque P Guenther D B Li L H Mazumdar A Straka C W August 2008 YREC the Yale rotating stellar evolution code Astrophysics and Space Science 316 1 4 31 41 arXiv 0710 4003 Bibcode 2008Ap amp SS 316 31D doi 10 1007 s10509 007 9698 y ISBN 978 1402094408 S2CID 14254892 a b 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 arXiv 1712 08109 Bibcode 2018AJ 155 30B doi 10 3847 1538 3881 aa9d8b S2CID 119427037 Aufdenberg J P et al 2008 Limb Darkening Getting Warmer In Richichi A Delplancke F Paresce F Chelli A eds The Power of Optical IR Interferometry Eso Astrophysics Symposia Vol 1 Berlin Springer pp 71 82 Bibcode 2008poii conf 71A doi 10 1007 978 3 540 74256 2 8 ISBN 978 3 540 74253 1 Langermann Y Tzvi 2018 Mathematics Astronomy and Astrology In Casagrande Kim Roberta Thrope Samuel Ukeles Raquel eds Romance and Reason Islamic Transformations of the Classical Past Princeton New Jersey Princeton University Press pp 92 93 ISBN 978 0 691 18184 4 a b Allen Richard Hinckley 1963 1899 Star Names Their Lore and Meaning Reprint ed New York Dover Publications Inc pp 312 313 ISBN 978 0 486 21079 7 Kunitzsch Paul 1959 Arabische Sternnamen in Europa in German Wiesbaden Otto Harrassowitz p 46 Kunitzsch P 1986 The Star Catalogue Commonly Appended to the Alfonsine Tables Journal for the History of Astronomy 17 2 89 98 Bibcode 1986JHA 17 89K doi 10 1177 002182868601700202 S2CID 118597258 Cleasby Richard Vigfusson Gudbrand 1874 An Icelandic English Dictionary Oxford United Kingdom Clarendon Press Taylor Douglas 1946 Notes on the Star Lore of the Caribbees American Anthropologist 48 2 215 222 doi 10 1525 aa 1946 48 2 02a00030 JSTOR 663691 Milbrath Susan 1999 Star Gods of the Maya Astronomy in Art Folklore and Calendars Austin Texas University of Texas Press p 39 ISBN 978 0 292 75226 9 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 amp Heritage 13 3 220 234 arXiv 1010 4610 Bibcode 2010JAHH 13 220H doi 10 3724 SP J 1440 2807 2010 03 06 S2CID 118454721 Harney Bill Yidumduma Cairns Hugh C 2004 2003 Dark Sparklers Revised ed Merimbula New South Wales Hugh C Cairns pp 139 140 ISBN 978 0 9750908 0 0 Parker Janet Mills Alice Stanton Julie 2007 Mythology Myths Legends and Fantasies New York Struik Publishers p 419 ISBN 978 1 77007 453 8 Archived from the original on 2 January 2014 Retrieved 3 November 2016 Kelley David H Milone Eugene F 2011 Exploring Ancient Skies A Survey of Ancient and Cultural Astronomy New York Springer p 341 ISBN 978 1 4419 7623 9 Best Elsdon 1922 Astronomical Knowledge of the Maori Genuine and Empirical Wellington New Zealand Dominion Museum pp 39 40 Archived from the original on 4 November 2012 Retrieved 16 November 2012 Renshaw Steve Ihara Saori October 1999 Yowatashi Boshi Stars that Pass in the Night Renshaw Works Retrieved 16 June 2020 Akira Matsumura 1988 大辞林 Daijirin in Japanese Tokyo Sanseidō ISBN 978 4 385 14001 8 Nojiri Hōei 2002 Shin seiza jyunrei Tokyo Chuokoron Shinsha p 19 ISBN 978 4 12 204128 8 MS Rigel Minnehallen The Memorial Hall in Norwegian Archived from the original on 4 February 2019 Retrieved 5 January 2019 Silverstone Paul H 1968 U S Warships of World War II Garden City New York Doubleday amp Company p 283 NH 1874 USS RIGEL AD 13 1922 46 Naval History and Heritage Command Retrieved 14 June 2020 80 G 1017252 USS Rigel AF 58 Naval History and Heritage Command Retrieved 14 June 2020 Yenne Bill 2018 The Complete History of U S Cruise Missiles Forest Lake Minnesota Specialty Press p 69 ISBN 978 1 58007 256 4 Antarctica Detail ID 12640 U S Geological Survey U S Department of the Interior Archived from the original on 2 February 2019 Retrieved 2 February 2019 Antarctica Detail ID 12639 U S Geological Survey U S Department of the Interior Retrieved 2 February 2019 External links Edit nbsp Wikimedia Commons has media related to Rigel NASA Astronomy Picture of the Day Rigel and the Witch Head Nebula 15 January 2018 NASA Astronomy Picture of the Day A Blazing Fireball between the Orion Nebula and Rigel 16 November 2015 December double star of the month beta Orionis Astronomical Society of Southern Africa My Favorite Double Star AAVSO Portals nbsp Astronomy nbsp Stars nbsp Outer space Retrieved from 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