Rigel

Coordinates: Sky map 05h 14m 32.272s, −08° 12′ 05.91″
Source: Wikipedia, the free encyclopedia.
For other uses, see Rigel (disambiguation).

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]
Distance
863[15][16] ly
(264 pc)
Absolute magnitude (MV)−7.84[9]
Orbit[12]
PrimaryA
CompanionBC
Period (P)24,000 yr
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
Myr
Ba
Mass3.84[12] M☉
Bb
Mass2.94[12] M☉
C
Mass3.84[12] M☉
BD−08°1063, FK5 194
B: Rigel B, GCRV 3111
Database references
SIMBADRigel
Rigel B

Rigel is a blue

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.

A star of

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 minute
, may be part of the same star system.

Nomenclature

Bright points of light against a dark background with wisps of colored nebulosity
Orion, with Rigel at bottom right, at optical wavelengths plus the Hα (hydrogen-alpha) spectral line to emphasize gas clouds

In 2016, the

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 (

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

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

Rigel is an

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

Rigel's

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

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

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

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

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

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

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 (

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

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

Rigel's distance from the Sun is somewhat uncertain, different estimates being obtained by different methods. Old estimates placed it 166 parsecs (or 541 light years) away from the Sun.

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

angular separation of 2.5° from the star,[56] 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).[58]

Rigel is an outlying member of the

runaway star with a complex history and might have originally formed in the main body of the association.[42]

Stellar system

The

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.

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.[57][63] 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.[64]

In 1871,

speckle interferometry showed the two almost identical components separated by 0.124″,[66] 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[65] or BU 555 in modern use.[8]

Component B is a double-lined

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,[63] 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,

″, 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.[67] 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.[63]

Physical characteristics

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

Rigel is a

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.[70] 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☉.[71] 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☉.[71] An older measurement of the angular diameter gives 2.75±0.01 mas,[72] 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] Older distance estimates were mostly far lower than modern estimates, leading to lower radius estimates; a 1922 estimate by John Stanley Plaskett gave Rigel a diameter of 25 million miles, or approximately 28.9 R☉, smaller than its neighbor Aldebaran.[73]

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

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.[69]

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.[69]

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

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"),[75] which can be traced to the 10th century.[76] "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][77] 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.[75]

With the constellation representing the mythological Greek huntsman

Aurvandil's toe" in Norse mythology.[78] 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).[79] The Lacandon people of southern Mexico knew it as tunsel ("little woodpecker").[80]

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.[81] The indigenous Boorong people of northwestern Victoria named Rigel as Collowgullouric Warepil.[82] 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.[83]

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.[85] Puaka is a southern name variant used in the South Island.[86]

In Japan, the Minamoto 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.[87][88][89]

In modern culture

The

US Navy that was cancelled in 1953 before reaching deployment.[94]

The

astrofix.[95] Mount Rigel, elevation 1,910 m (6,270 ft), is also in Antarctica.[96]

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

Notes

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  2. ^ lit."... and it is called Algebar. It is also named Rigel."

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External links

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