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Revision as of 07:35, 9 February 2019

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

Rigel (/ˈraɪdʒəl, -ɡəl/), also designated β Orionis (Latinized to Beta Orionis, abbreviated Beta Ori, β Ori), is on average the seventh-brightest star in the night sky and the brightest in the constellation of Orion—though occasionally it is outshone within the constellation by the variable star Betelgeuse. It is a luminous object some 863 light-years distant from Earth, varying irregularly between apparent magnitude +0.05 and +0.18.

Rigel as seen from Earth is actually a multiple star system of three to five stars. A companion, Rigel B, is 500 times fainter than the supergiant Rigel A and visible only with a telescope. Rigel B is itself a multiple star system, including a spectroscopic pair and a visual companion C. Component C, with a very similar brightness and spectrum to B, is probably not the spectroscopic companion, making the system a triple star.

The primary star, Rigel A, is a blue-white supergiant estimated to be anywhere from 61,500 to 363,000 times as luminous as the Sun, depending on the method used to calculate its properties and assumptions about its distance. It has exhausted the hydrogen in its core and expanded to over 70 times the Sun's radius. It pulsates quasi-periodically and is classified as an Alpha Cygni variable.

Nomenclature

Rigel and reflection nebula IC 2118 in Eridanus. Rigel B is not visible in the glare of the main star.

The name Rigel was likely first recorded in the Alfonsine Tables of 1252. It is derived from the Arabic name Rijl Jauzah al Yusrā, "the left leg (foot) of Jauzah" (i.e. rijl meaning "leg, foot"),[17] which can be traced to the 10th century.[18] "Jauzah" was a proper name of the Orion figure, an alternative Arabic name was رجل الجبار riǧl al-ǧabbār, "the foot of the great one", which is the source of the rarely used variant names Algebar or Elgebar. The Alphonsine Tables saw its name split into "Rigel" and "Algebar", with the note, et dicitur Algebar. Nominatur etiam Rigel.[19] Alternate spellings from the 17th century include Regel by Italian astronomer Giovanni Battista Riccioli, Riglon by German astronomer Wilhelm Schickard, and Rigel Algeuze or Algibbar by English scholar Edmund Chilmead.[17]

In 2016, the name Rigel was officially entered in the IAU Catalog of Star Names for β Orionis A, the blue supergiant component visible to the naked eye.[20]

Beta Orionis is the star's Bayer designation, although it is usually the brightest star in Orion. Astronomer James B. Kaler has speculated that perhaps Rigel was named by Bayer during a rare period where it was outshone by the variable Betelgeuse, resulting in the latter star being designated Alpha and Rigel Beta Orionis.[21]

Observation

Rigel is the seventh-brightest star in the celestial sphere excluding the Sun—usually fainter than Capella,[22] although both are slightly variable in brightness. Rigel is an irregular pulsating variable with a visual range of magnitude 0.05–0.18. Although Rigel has the Bayer designation "beta", it is almost always brighter than Alpha Orionis (Betelgeuse).[22]

Since 1943, the spectrum of this star has served as the spectral reference, for class B8Ia, by which other stars are classified.[23][24] Rigel has a color index (B–V) of −0.06, meaning it appears slightly blue-white, almost white.[25]

Culminating at midnight on 12 December, and at 9 pm on 24 January, Rigel is most visible in winter evenings in the northern hemisphere and summer in the southern.[22] In the southern hemisphere, Rigel is the first bright star of Orion visible as the constellation rises.[26]

In stellar navigation, Rigel is one of the most important navigation stars, since it is bright, easily located and equatorial, which means it is visible all around the world's oceans (the exception, areas within 8° of the North Pole).[27]

Spectroscopy

The general spectral type of Rigel as B8 is well-established and it has been used as a defining point of the spectral classification sequence for supergiants.[28][29] The overall spectrum is typical for a late B class star, with strong absorption lines of the hydrogen Balmer series together with neutral helium lines and some of heavier elements such as oxygen, calcium, and magnesium.[30] The luminosity class for B8 stars is determined from the strength and narrowness of the hydrogen spectral lines, and Rigel is assigned to the bright supergiant class Ia.[23]

As early as 1888, the radial velocity of Rigel, as determined from the Doppler shifts of its spectral lines, was seen to vary. This was confirmed and interpreted as a spectroscopic companion with a period of about 22 days.[31] The radial velocity has since been measured to vary by about km/s around a mean of 21 km/s.[32]

In 1933, the Hα spectral line was seen to be unusually weak and shifted 0.1 nm towards shorter wavelengths, while there was a narrow emission spike about 1.5 nm to the long wavelength side of the main absorption line.[33] This is now known as a P Cygni profile after a star that shows this feature strongly in its spectrum. It is associated with strong mass loss where there is simultaneously emission from dense wind close to the star and absorption from circumstellar material expanding away from the star.[33]

The unusual Hα line profile has since been 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.[32] 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 are seen, and even more rarely infalling material. The overall picture is one of large looping structures arising from the photosphere and driven by magnetic fields.[34]

The variations in the spectrum have been reflected in published spectral classes, such as B8 Ia, B8 Iab, and B8 Iae.[13][35]

Variability

Rigel has been known to vary in brightness since at least 1930, although the exact range and type of variability was unclear. Published results showed variations of less than 0.1 magnitudes with no obvious period. Observations 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. The colour index also varied but in general was not strongly correlated with the brightness variations.[36]

From an analysis of Hipparcos satellite photometry, Rigel was identified as belonging to the Alpha Cygni class of variable star in 1998.[37] It was added to the General Catalogue of Variable Stars in the following year in the 74th namelist of variable stars.[38] The Hipparcos photometry showed variations with a photographic amplitude of 0.039 magnitudes and a possible period of 2.075 days.[39]

Rigel was observed with the Canadian MOST satellite for nearly 28 days in 2009. The light variations in this supergiant star were at the milli-magnitude level. The gradual changes in the flux highlights the presence of long-period pulsation modes in the star.[14]

Mass loss

By observing the Hα spectral line, Chesneau and colleagues calculated the mass loss from Rigel to be (1.5±0.4)×10−7 solar masses per year (M☉/yr)in 2009, around ten million times more than the mass loss from the Sun.[40]

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 spectral line profiles, and measurement of the regions producing the lines, show that the stellar wind varies greatly in structure and strength. Loop and arm structures were also detected within the wind. Calculations of mass loss from the Hγ line give (9.4±0.9)×10−7 M☉/yr in 2006-7 and (7.6±1.1)×10−7 M☉/yr in 2009-10. Calculations using the Hα line give lower results, around 1.5×10−7 M☉/yr.[41]

Distance

The distance to Rigel has been difficult to determine with any accuracy, as its brightness is not easy to determine independently and its is somewhat too distant for very accurate parallax measurements. As it is both bright and moving through a region of nebulosity, Rigel lights up several dust clouds in its vicinity, most notably IC 2118 (the Witch Head Nebula).[42] These are thought to be about 40 light-years (12 parsecs) distant from the star itself.[21] Rigel has been classified as an outlying member of the Orion OB1 Association at a distance of up to 1,600 light-years (500 parsecs). It has also been listed as a member of the poorly-defined Taurus-Orion R1 Association, somewhat closer at 1,200 light-years (360 parsecs).[43][44] It is thought to be considerably closer than most of the members of Orion OB1 and the Orion Nebula, but projecting Rigel's path through space for its expected age brings it close to the nebula. Betelgeuse and Saiph lie at a similar distance to Rigel, although Betelgeuse is a runaway star with a complex history and is likely to have originally formed in the main body of the association.[35]

The revised 2007 Hipparcos reduction of Rigel's parallax gives a distance of 863 light-years (265 parsecs), with a margin of error of about 9%.[2]

A companion star to Rigel, usually considered to be physically associated and at the same distance, has a Gaia Data Release 2 parallax of 2.9186±0.0761 mas, implying a distance around 1,100 light-years (340 parsecs) but the measurements show a number of features suggesting they may be unreliable, possibly because it is a close double star.[45]

Stellar system

Rigel has been known as a visual double star since at least 1822, when it was measured by Friedrich Georg Wilhelm von Struve.[46] The companion is not particularly faint at magnitude 6.7, and with a separation of 9.5 arc seconds both components are resolvable in most amateur astronomers' telescopes.[46] However, the large difference in brightness makes it a challenging target for telescope apertures smaller than 15.0 cm (5.9 in). The companion is frequently referred to as Rigel B, but more correctly as β Orionis B or by a multiple star designation such as ADS 3823 B.[47] Through a telescope, it is around 9" south of Rigel itself.[48]

At Rigel's estimated distance, Rigel B's projected separation from its primary is over 2,200 AU. Since its discovery, there has been no sign of orbital movement, although both stars share similar common proper motion.[49][42] The pair would have a minimum orbital period of around 18,000 years.[7] Gaia Data Release 2 (DR2) contains a somewhat unreliable parallax for Rigel B placing it at about 1,100 light-years (340 parsecs), further away than the Hipparcos distance for Rigel, but similar to the Taurus-Orion R1 association. There is no parallax for Rigel in Gaia DR2. The Gaia DR2 proper motions for Rigel B and the Hipparcos proper motions for Rigel are both small, although not quite the same.[45]

Since the 19th century, Rigel B has been reported to be resolved into a close binary of two equal components, with the measured separation varying from less than 0.1" to nearly 0.2". Speckle interferometry showed in 2009 two almost identical components separated by 0.124".[50] The companion is designated as component C. Both stars have apparent visual magnitudes of 7.6 with a likely orbital period of 63 years.[7]

Rigel B itself appears to be a spectroscopic binary system, consisting of two main sequence stars that orbit each other every 9.86 days. These two stars do not seem to correspond to the visual binary components of B or C, so the BC sub-system might be a triple, although the true arrangement is unclear.[49]

Multiple star catalogs include a 15th magnitude star at 44.6″ and position angle of 1°, catalogued as component D, although it is unclear whether it is physically related or a coincidental alignment.[46] Gaia DR2 finds it to be a 12th magnitude sunlike star at approximately the same distance as Rigel.[51] A spectroscopic companion to Rigel has been reported on the basis of radial velocity variations, and even an orbit calculated, but it is thought that the star does not exist and the pulsations are intrinsic to Rigel itself.[49]

Physical characteristics

File:Hertzsprung-Russel StarData.png
Rigel's place at top center on the Hertzsprung-Russell diagram

Rigel is the most luminous star within 1000 light-years of the Sun.[22] Moravveji and colleagues calculate a luminosity for Rigel A of 120,000 times that of the Sun.[14] Its surface temperature is around 12,100 K. The interferometer-measured angular diameter of this star, after correction for limb darkening, is 2.75±0.01 mas.[52] At its estimated distance, this yields a size of about 78.9 times the radius of the Sun (R☉).[14] Norbert Przybilla and colleagues assumed a distance of 1,170 ± 130 light-years (360 ± 40 parsecs). They calculated it to be around 218,000 times as luminous as the Sun, and have around 21±3 solar masses and 109±12 R☉.[8]

A 2018 study using the Navy Precision Optical Interferometer came up with an angular diameter of 2.606±0.009 mas, yielding a radius of 74.1+6.1
−7.3 R☉, and luminosity 61,515±11,486 times that of the Sun.[53] Based on the Hipparcos distance of 780 light-years (240 parsecs) and an Orion OB1 association distance of 1,600 light-years (500 parsecs), the luminosity is calculated to be somewhere between 83,000 L☉ and 363,000 L☉[43]

Rigel is a blue supergiant that has exhausted burning the hydrogen fuel in its core and left the main sequence, expanded, and brightened as it progresses across the Hertzsprung–Russell diagram. Some studies suggest it has already passed though a phase as a red supergiant.[54] Przybilla estimated that it has lost around 3 solar masses since beginning life as a star of 24±3 solar masses 7 to 9 million years ago.[8] It is expected to eventually end its stellar life by exploding as a type II supernova from a red supergiant, in the process flinging out material that will serve to seed future generations of stars.[10] It is one of the closest known potential supernova progenitors to Earth,[14] and would be expected to have an apparent magnitude of around −11 at its peak.[4]

Rigel's variability is complex and is caused by stellar pulsations similar to those of Deneb, the prototype of the class of Alpha Cygni pulsating stars. The radial velocity variations of Rigel prove that it simultaneously oscillates in at least 19 non-radial modes with periods ranging from about 1.2 to 74 days.[14] While its pulsations are powered by the nuclear reactions in a hydrogen-burning shell that is at least partially non-convective, the star also burns helium in its core.[10]

The companions Rigel Ba, Bb, and C all appear to be similar B class main sequence stars of 3 - 4 M☉, but their properties are not accurately known.[7]

Etymology and cultural significance

In ancient Egypt, Rigel's is thought to have been called Seba-en-Sah Sb3-n-S3ḥ, which means Star of Sah.[55] In heiroglyphics, this is
S29Aa17V28D61N14
N35

Rigel is thought to denote either Orion's knee or (as its name suggests) his foot; the nearby star Beta Eridani marking the footstool.[22] Rigel is presumably the star known as "Aurvandil's toe" in Norse mythology.[56]

In Chinese, 參宿 (Shēn Sù), meaning Three Stars (asterism), refers to an asterism consisting of Rigel, Alnitak, Alnilam, Mintaka, Betelgeuse, Bellatrix and Saiph.[57] Consequently, Rigel are known as 參宿七 (Shēn Sù qī, the Seventh Star of Three Stars).[58]

In Japan, the Minamoto or Genji clan chose Rigel and its white color as its symbol, calling the star Genji-boshi (源氏星), while the Taira or Heike clan adopted Betelgeuse and its red color. The two powerful families fought a legendary war in Japanese history, the stars seen as facing each other off and only kept apart by the Belt.[59][60][61] Rigel was also known as Gin-waki, (銀脇), "the Silver (Star) beside (Mitsu-boshi)".

Rigel was known as Yerrerdet-kurrk to the Wotjobaluk koori of southeastern Australia, and held to be the mother-in-law of Totyerguil (Altair). The distance between them signified the taboo preventing a man from approaching his mother-in-law.[62] The indigenous Boorong people of northwestern Victoria named Rigel as Collowgullouric Warepil.[63] The Wardaman people of northern Australia know Rigel as the Red Kangaroo Leader Unumburrgu and chief conductor of ceremonies in a songline when Orion is high in the sky. The river Eridanus marks a line of stars in the sky leading to it, and the other stars of Orion are his ceremonial tools and entourage. Betelgeuse is Ya-jungin "Owl Eyes Flicking", watching the ceremonies.[64]

The Māori people named Rigel as Puanga, which was said to be a daughter of Rehua (Antares), the chief of all stars.[65] Its heliacal rising also presaged the appearance of Matariki (the Pleiades) in the dawn sky which marked the Māori New Year in late May or early June. The Moriori people of the Chatham Islands, as well as some Maori groups in New Zealand, marked the start of their New Year with Rigel rather than the Pleiades.[66] Puaka was a local variant used in the South Island.[67]

In the Caribbean, Rigel represented the severed leg of the folkloric figure Trois Rois, himself represented by the three belt stars of Orion. The leg had been severed with a cutlass by the maiden Bįhi (Sirius).[68] The Lacandon people of southern Mexico knew it as tunsel ("little woodpecker").[69]

In modern culture

Rigel and escort under attack

The MS Rigel was originally a Norwegian ship, built in Copenhagen in 1924. It was requisitioned by the Germans during the second World War and sunk in 1944 while being used to transport prisoners of war.[70] Two US Navy ships have borne the name USS Rigel after the star.

The SSM-N-6 Rigel, named after the star, was a cruise missile program for the US Navy that was cancelled before reaching deployment.

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.[71] Mount Rigel, also in Antarctica, is also named after the star.[72]

The name Rigel, or the star itself, occurs frequently in fictional works.

References

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External links

source: https://en.wikipedia.org/w/index.php?title=Rigel&type=revision&diff=882462204&oldid=882403242

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