Auriga (constellation)

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Auriga
Constellation
Auriga
AbbreviationAur[1]
GenitiveAurigae
Pronunciation
Symbolismthe
Capella (α Aur) (0.08m)
Messier objects3[5]
Meteor showers
Bordering
constellations
Visible at latitudes between +90° and −40°.
Best visible at 21:00 (9 p.m.) during the month of late February to early March.

Auriga is a constellation in the

88 modern constellations; it was among the 48 constellations listed by the 2nd-century astronomer Ptolemy. Its name is Latin for '(the) charioteer', associating it with various mythological beings, including Erichthonius and Myrtilus. Auriga is most prominent during winter evenings in the northern Hemisphere, as are five other constellations that have stars in the Winter Hexagon asterism. Because of its northern declination, Auriga is only visible in its entirety as far south as -34°; for observers farther south it lies partially or fully below the horizon. A large constellation, with an area of 657 square degrees, it is half the size of the largest, Hydra
.

Its brightest star,

Flaming Star Nebula, associated with the variable star AE Aurigae
.

In Chinese mythology, Auriga's stars were incorporated into several constellations, including the celestial emperors' chariots, made up of the modern constellation's brightest stars. Auriga is home to the radiant for the Aurigids, Zeta Aurigids, Delta Aurigids, and the hypothesized Iota Aurigids.

History and mythology

The first record of Auriga's stars was in Mesopotamia as a constellation called GAM, representing a scimitar or crook. However, this may have represented just Capella (Alpha Aurigae) or the modern constellation as a whole; this figure was alternatively called Gamlum or MUL.GAM in the MUL.APIN. The crook of Auriga stood for a goat-herd or shepherd. It was formed from most of the stars of the modern constellation; all of the bright stars were included except for Elnath, traditionally assigned to both Taurus and Auriga. Later, Bedouin astronomers created constellations that were groups of animals, where each star represented one animal. The stars of Auriga comprised a herd of goats, an association also present in Greek mythology.[8] The association with goats carried into the Greek astronomical tradition, though it later became associated with a charioteer along with the shepherd.[9]

In Greek mythology, Auriga is often identified as the mythological Greek hero Erichthonius of Athens, the chthonic son of Hephaestus who was raised by the goddess Athena. Erichthonius was generally credited to be the inventor of the quadriga, the four-horse chariot, which he used in the battle against the usurper Amphictyon, the event that made Erichthonius the king of Athens.[10][11] His chariot was created in the image of the Sun's chariot, the reason Zeus placed him in the heavens.[12] The Athenian hero then dedicated himself to Athena and, soon after, Zeus raised him into the night sky in honor of his ingenuity and heroic deeds.[13]

A painting by Peter Paul Rubens entitled Finding of Erichthonius; Erichthonius and Auriga are often associated.

Auriga, however, is sometimes described as

Hippolytus. He was ejected from Athens after he refused the romantic advances of his stepmother Phaedra, who committed suicide as a result. He was killed when his chariot was wrecked, but revived by Asclepius.[12][14]

Auriga is also said to represent Phaethon, son of the sun Helios, who tricked his father into letting him drive his chariot for a day. Phaethon crashed and burned, scorching the earth. He was then placed in the night sky as the Auriga.[15] Regardless of Auriga's specific representation, it is likely that the constellation was created by the ancient Greeks to commemorate the importance of the chariot in their society.[16]

An incidental appearance of Auriga in Greek mythology is as the limbs of Medea's brother. In the myth of Jason and the Argonauts, as they journeyed home, Medea killed her brother and dismembered him, flinging the parts of his body into the sea, represented by the Milky Way. Each individual star represents a different limb.[17]

Titans' defeat, because Zeus skinned the goat and wore it as his aegis.[12] The asterism containing the goat and kids had been a separate constellation; however, Ptolemy merged the Charioteer and the Goats in the 2nd-century Almagest.[16] Before that, Capella was sometimes seen as its own constellation—by Pliny the Elder and Manilius—called Capra, Caper, or Hircus, all of which relate to its status as the "goat star".[19] Zeta Aurigae and Eta Aurigae were first called the "Kids" by Cleostratus, an ancient Greek astronomer.[12]

Auriga carrying the goat and kids as depicted in Urania's Mirror, a set of constellation cards illustrated by Sidney Hall, London c. 1825.

Traditionally, illustrations of Auriga represent it as a chariot and its driver. The charioteer holds a goat over his left shoulder and has two

Hyginus deviated from this typical depiction by showing a four-wheeled cart driven by Auriga, who holds the reins of two oxen, a horse, and a zebra. Jacob Micyllus depicted Auriga in his Hyginus of 1535 as a charioteer with a two-wheeled cart, powered by two horses and two oxen. Arabic and Turkish depictions of Auriga varied wildly from those of the European Renaissance; one Turkish atlas depicted the stars of Auriga as a mule, called Mulus clitellatus by Johann Bayer.[19] One unusual representation of Auriga, from 17th-century France, showed Auriga as Adam kneeling on the Milky Way, with a goat wrapped around his shoulders.[20]

Occasionally, Auriga is seen not as the Charioteer but as

Jupiter pitied Bellerophon for his foolishness and placed him in the stars.[21]

Johann Bode combined Hell's constellations into Telescopium Herschelii in 1801, located mostly in Auriga.[23]

Since the time of Ptolemy, Auriga has remained a constellation and is officially recognized by the

Eugène Delporte as a polygon of 20 segments. Its right ascension is between 4h 37.5m and 7h 30.5m and its declination is between 27.9° and 56.2° in the equatorial coordinate system.[3]

In non-Western astronomy

The stars of Auriga were incorporated into several Chinese constellations. Wuche, the five chariots of the celestial emperors and the representation of the grain harvest, was a constellation formed by Alpha Aurigae, Beta Aurigae, Beta Tauri, Theta Aurigae, and Iota Aurigae. Sanzhu or Zhu was one of three constellations which represented poles for horses to be tethered. They were formed by the triplets of Epsilon, Zeta, and Eta Aurigae; Nu, Tau, and Upsilon Aurigae; and Chi and 26 Aurigae, with one other undetermined star. Xianchi, the pond where the sun set and Tianhuang, a pond, bridge, or pier, were other constellations in Auriga, though the stars that composed them are undetermined. Zuoqi, representing chairs for the emperor and other officials, was made up of nine stars in the east of the constellation. Bagu, a constellation mostly formed from stars in Camelopardalis representing different types of crops, included the northern stars of Delta and Xi Aurigae.[12]

In ancient

Hindu astronomy, Capella represented the heart of Brahma and was important religiously. Ancient Peruvian peoples saw Capella, called Colca, as a star intimately connected to the affairs of shepherds.[20]

In Brazil, the

Aztec people, as the Late Classic site Monte Albán has a marker for the star's heliacal rising.[28] Indigenous peoples of California and Nevada also noticed the bright pattern of Auriga's stars. To them, the constellation's bright stars formed a curve that was represented in crescent-shaped petroglyphs.[29] The indigenous Pawnee of North America recognized a constellation with the same major stars as modern Auriga: Alpha, Beta, Gamma (Beta Tauri), Theta, and Iota Aurigae.[30]

The people of the

Scorpius represents Dümur, the oldest son of the stars' mother, and the Pleiades represent her youngest son. The mother of the stars, Ligedaner,[31][32] is represented by Capella; she lived on the island of Alinablab. She told her sons that the first to reach an eastern island would become the King of the Stars, and asked Dümur to let her come in his canoe. He refused, as did each of her sons in turn, except for Pleiades. Pleiades won the race with the help of Ligedaner, and became the King of the Stars.[31] Elsewhere in the central Caroline Islands, Capella was called Jefegen uun (variations include efang alul, evang-el-ul, and iefangel uul), meaning "north of Aldebaran".[33] Different names were noted for Auriga and Capella in Eastern Pacific societies. On Pukapuka, the figure of modern Auriga was called Te Wale-o-Tutakaiolo ("The house of Tutakaiolo");[34] in the Society Islands, it was called Faa-nui ("Great Valley").[35] Capella itself was called Tahi-anii ("Unique Sovereign") in the Societies.[36] Hoku-lei was the name for Capella but may have been the name for the whole constellation; the name means "Star-wreath" and refers to one of the wives of the Pleiades, called Makalii.[37]

The stars of Auriga feature in

Alshain (Beta Aquilae), would rise soon. Aagjuuk, which represented the dawn following the winter solstice, was an incredibly important constellation in the Inuit mythos.[39] It was also used for navigation and time-keeping at night.[40]

Features

The constellation Auriga as it can be seen by the naked eye.

Stars

A size comparison of the four stars in the Capella system and the Sun.

Bright stars

Mt. Wilson Observatory telescope. It appears with a golden-yellow hue, though Ptolemy and Giovanni Battista Riccioli both described its color as red, a phenomenon attributed not to a change in Capella's color but to the idiosyncrasies of their color sensitivities.[42] Capella has an absolute magnitude of 0.3 and a luminosity of 160 times the luminosity of the Sun, or 160 L (the primary is 90 L and the secondary is 70 L).[45] It may be loosely associated with the Hyades, an open cluster in Taurus, because of their similar proper motion. Capella has one more companion, Capella H, which is a pair of red dwarf stars located 11,000 astronomical units (0.17 light-years) from the main pair.[42]

common proper motion. This 14th-magnitude star was discovered in 1901 by Edward Emerson Barnard. It has a separation of 12.6 arcseconds, and is around 350 astronomical units from the primary.[42]

Other bright stars

Besides particularly bright stars of Alpha and Beta Aurigae, Auriga has many dimmer naked-eye visible stars.

Gamma Aurigae, now known under its once co-name

B7III class star (B-type giant).[49] At about +1.65 it would rank a clear third in apparent magnitude if still co-placed in Auriga.[10][18] It is a mercury-manganese star, with some large signatures of heavy elements.[50]

hybrid star, an x-ray producing giant star that emits x-rays from its corona and has a cool stellar wind.[52][53] Though its proper motion is just 0.02 arcseconds per year, it has a radial velocity of 10.5 miles (16.9 km) per second in recession.[42] The traditional name Kabdhilinan, sometimes shortened to "Alkab", comes from the Arabic phrase al-kab dh'il inan, meaning "shoulder of the rein holder". Iota may end as a supernova, but because it is close to the mass limit for such stars, it may instead become a white dwarf.[52]

Delta Aurigae, the northernmost bright star in Auriga,[54] is a K0III-type star (K-type giant),[45][54][55] 126 light-years from Earth[55] and approximately 1.3 billion years old.[54] It has a magnitude of 3.72, an absolute magnitude of 0.2, and a luminosity of 60 L.[45] About 12 times the radius of the Sun, Delta weighs only two solar masses and rotates with a period of almost one year.[54] Though it is often listed as a single star,[56] it actually has three very widely spaced optical companions. One is a double star of magnitude 11, two arcminutes apart; the other is a star of magnitude 10, three arcminutes apart.[54]

hydrogen-fusing lifespan at an age of 6.2 billion years. It also has an unusually high radial velocity at 83 km/second. Though older than the Sun, it is similar in many ways; its mass is 1.07 solar masses, a radius of 1.3 solar radii, and a rotational period of 26 days. However, it differs from the Sun in its metallicity; its iron content is 1.15 times that of the Sun and it has relatively less nitrogen and carbon. Like Delta, it has several optical companions and is often categorized as a single star. The brightest companions are of magnitude 10, separated by 175 and 203 arcseconds. The dimmer companions are of magnitude 13 and 14, 87 and 310 arcseconds from Lambda, respectively.[61]

Nu Aurigae is a G9.5III (G-type giant)[62] star of magnitude 3.97,[45] 230 light-years from Earth.[62] It has a luminosity of 60 L and an absolute magnitude of 0.2.[45] Nu is a giant star with a radius of 20–21 solar radii and a mass of approximately 3 solar masses. It may technically be a binary star; its companion, sometimes listed as optical and separated by 56 arcseconds, is a dwarf star of spectral type K6 and magnitude 11.4. Its period is more than 120,000 years and it orbits at least 3,700 AU from the primary.[54]

Star Spectral
class
Apparent
magnitude[45]
Absolute
magnitude[45]
Distance
(light-years)
Kappa Aurigae G8.5IIIb[63] 4.25 0.3 177[63]
Pi Aurigae M3II[64] 4.26 −2.4 758[64]
Tau Aurigae G8III[65] 4.52 0.3 206[65]
Upsilon Aurigae M0III[66] 4.74 −0.5 526[66]
Chi Aurigae B4Ib[67] 4.76 −6.3 3032[45]
2 Aurigae K3III[68] 4.78 −0.2 604[68]
Mu Aurigae A4m[69] 4.86 1.8 153[69]
Sigma Aurigae K4III[70] 4.89 −0.3 466[70]
Omega Aurigae A1V[71] 4.94 0.6 171[71]
Xi Aurigae A2V[72] 4.99 0.8 233[72]
9 Aurigae F0V[73] 5.00 2.6 86[73]

Eclipsing binary stars

An artist's rendering of the Epsilon Aurigae system.

The most prominent variable star in Auriga is

white supergiant, and the secondary may be itself a binary star within a large dusty disk. Its maximum magnitude is 3.0, but it stays at a minimum magnitude of 3.8 for around a year; its most recent eclipse began in 2009.[18] The primary has an absolute magnitude of −8.5 and an unusually high luminosity of 200,000 L, the reason it appears so bright at such a great distance.[45] Epsilon Aurigae is the longest-period eclipsing binary currently known.[10] The first observed eclipse of Epsilon Aurigae occurred in 1821, though its variable status was not confirmed until the eclipse of 1847–48. From that time forward, many theories were put forth as to the nature of the eclipsing component. Epsilon Aurigae has a noneclipsing component, which is visible as a 14th magnitude companion separated from the primary by 28.6 arcseconds. It was discovered by Sherburne Wesley Burnham in 1891 at the Dearborn Observatory, and is about 0.5 light-years from the primary.[42]

Another eclipsing binary in Auriga, part of the Haedi asterism with Eta Aurigae, is

B3 class star located 243 light-years from Earth[76] with a magnitude of 3.17.[10] It is a B3V class star, meaning that it is a blue-white hued main-sequence star.[42][76] Eta Aurigae has an absolute magnitude of −1.7 and a luminosity of 450 L.[45] Eta Aurigae is moving away from Earth at a rate of 4.5 miles (7.2 km) per second.[42]

Nova Aquilae 1918, it is a very close binary with a very short period. T Aurigae's period of 4.905 hours is comparable to DQ Herculis's period of 4.65 hours, and it has a partial eclipse period of 40 minutes.[42]

Other variable stars

There are many other variable stars of different types in Auriga.

emission lines of calcium and hydrogen.[42] Its spectral type is G5V:e.[82] SS Aurigae is an SS Cygni-type variable star, classified as an explosive dwarf. Discovered by Emil Silbernagel in 1907, it is almost always at its minimum magnitude of 15, but brightens to a maximum up to 60 times brighter than the minimum an average of every 55 days, though the period can range from 50 days to more than 100 days. It takes about 24 hours for the star to go from its minimum to maximum magnitude. SS Aurigae is a very close binary star with a period of 4 hours and 20 minutes. Both components are small subdwarf stars; there has been dispute in the scientific community about which star originates the outbursts.[42] UU Aurigae is a variable red giant star at a distance of 2,000 light-years. It has a period of approximately 234 days and ranges between magnitudes 5.0 and 7.0.[18]

The Flaming Star Nebula (IC 405), and its neighbor IC 410, along with AE Aurigae, which illuminates the nebula.

runaway star" from the young cluster in the Orion Nebula, leaving the cluster approximately 2.7 million years ago. It is similar to 53 Arietis and Mu Columbae, other runaway stars from the Orion cluster.[42] Its spectral class is O9.5Ve, meaning that it is an O-type main-sequence star.[83] The Flaming Star Nebula, is located near IC 410 in the celestial sphere. IC 410 obtained its name from its appearance in long exposure astrophotographs; it has extensive filaments that make AE Aurigae appear to be on fire.[84]

There are four Mira variable stars in Auriga: R Aurigae, UV Aurigae, U Aurigae, and X Aurigae, all of which are type M stars.[45] More specifically, R Aurigae is of type M7III,[85] UV Aurigae is of type C6 (a carbon star),[86] U Aurigae is of type M9,[87] and X Aurigae is of type K2.[88] R Aurigae, with a period of 457.5 days, ranges in magnitude from a minimum of 13.9 to a maximum of 6.7. UV Aurigae, with a period of 394.4 days, ranges in magnitude from a minimum of 10.6 to a maximum of 7.4. U Aurigae, with a period of 408.1 days, ranges in magnitude from a minimum of 13.5 to a maximum of 7.5. X Aurigae, with a particularly short period of 163.8 days, ranges in magnitude from a minimum of 13.6 to a maximum of 8.0.[45]

Binary and double stars

Auriga is home to several less prominent binary and double stars.

optical binary star. The primary is of magnitude 5.0 and is at a distance of 270 light-years; the secondary is of magnitude 7.9 and is at a distance of 82 light-years.[18] HD 30453 is spectroscopic binary of magnitude 5.9, with a spectral type assessed as either A8m or F0m, and a period of seven days.[91][92]

Stars with planetary systems

There are several stars with confirmed planetary systems in Auriga; there is also a white dwarf with a suspected planetary system.

spectral class F8V star of magnitude 6.74 — just past the limit of visibility to the naked eye. It is of similar size to the Sun, at 1.1 solar masses and 1.21 solar radii. The planet, with a mass of 3.83 Jupiter masses, orbits with a semi-major axis of 0.83 AU and a period of 263.1 days.[94] HD 45350 has one planet as well.[95][96] HD 45350 b was discovered through radial velocity measurements in 2004. It has a mass of 1.79 Jupiter masses and orbits every 890.76 days at a distance of 1.92 AU. Its parent star is faint, at an apparent magnitude of 7.88, a G5IV type star 49 parsecs away. It has a mass of 1.02 solar masses and a radius of 1.27 solar radii.[97] HD 43691 b is a significantly larger planet, with a mass of 2.49 Jupiter masses; it is also far closer to its parent star, HD 43691. Discovered in 2007 from radial velocity measurements,[98]
it orbits at a distance of 0.24 AU with a period of 36.96 days.[99][100] HD 43691 has a radius identical to the Sun's, though it is more dense—its mass is 1.38 solar masses. It is a G0IV type star of magnitude 8.03, 93.2 parsecs from Earth.[101]

transit method in 2008.[105] It has a mass of 0.67 Jupiter masses and orbits just 0.053 AU from its parent star, with a period of 3.92 days; its radius is 1.4 Jupiter radii, making it a hot Jupiter. Its parent star, HAT-P-9, is an F-type star[105] approximately 480 parsecs from Earth. It has a mass of 1.28 solar masses and a radius of 1.32 solar radii.[106]

The star

binary star system KELT-2. KELT-2B is an early K-dwarf about 295 AU away, and was discovered the same time as the exoplanet.[107]

Deep-sky objects

Auriga has the

runaway star, is a bright variable star currently within the Flaming Star Nebula.[42]

A photograph of M36, clearly showing its characteristic knot of bright stars and its concentration

M36 (NGC 1960) is a young galactic open cluster with approximately 60 stars, most of which are relatively bright; however, only about 40 stars are visible in most amateur instruments.

Trumpler class is given as both I 3 r and II 3 m. Besides the central knot, most of the cluster's other stars appear in smaller knots and groups.[90]

A photograph of M37, showing its obviously larger size and its notable brightness

M37 (NGC 2099) is an open cluster, larger than M36 and at a distance of 4,200 light-years. It has 150 stars, making it the richest cluster in Auriga; the most prominent member is an orange star that appears at the center.

A type stars, though there are at least 12 red giants in the cluster as well.[42] M37's Trumpler class is given as both I 2 r and II 1 r. The stars visible in a telescope range in magnitude from 9.0 to 13.0; there are two 9th magnitude stars in the center of the cluster and an east to west chain of 10th and 11th magnitude stars.[90]

A photograph of M38; its characteristic shape, clearly visible to an observer in a telescope, is obscured by the greater number of stars revealed by a long-exposure photograph.

M38 is a diffuse open cluster at a distance of 3,900 light-years, the least concentrated of the three main open clusters in Auriga;

G type giant stars. One yellow-hued G type star is the brightest star in M38 at a magnitude of 7.9.[42] The brightest stars in M38 are magnitude 9 and 10.[90] M38 is accompanied by NGC 1907, a smaller and dimmer cluster that lies half a degree south-southwest of M38; it is at a distance of 4,200 light-years.[18] The smaller cluster has an overall magnitude of 8.2 and a diameter of 6.0 arcminutes, making it about a third the size of M38. However, NGC 1907 is a rich cluster, classified as a Trumpler Class I 1 m n cluster. It has approximately 12 stars of magnitude 9–10, and at least 25 stars of magnitude 9–12.[90]

IC 410, a faint nebula, is accompanied by the bright open cluster NGC 1893. The cluster is thin, with a diameter of 12 arcminutes and a population of approximately 20 stars. Its accompanying nebula has very low surface brightness, partially because of its diameter of 40 arcminutes. It appears in an amateur telescope with brighter areas in the north and south; the brighter southern patch shows a pattern of darker and lighter spots in a large instrument.[109] NGC 1893, of magnitude 7.5, is classified as a Trumpler Class II 3 r n or II 2 m n cluster, meaning that it is not very large and is somewhat bright. The cluster possesses approximately 30 stars of magnitude 9–12. In an amateur instrument, IC 410 is only visible with an Oxygen-III filter.[90] NGC 2281 is a small open cluster at a distance of 1,500 light-years. It contains 30 stars in a crescent shape.[18] It has an overall magnitude of 5.4 and a fairly large diameter of 14.0 arcseconds, classified as a Trumpler Class I 3 m cluster. The brightest star in the cluster is magnitude 8; there are approximately 12 stars of magnitude 9–10 and 20 stars of magnitude 11–13.[90]

A picture of NGC 1893 obtained by the Spitzer Space Telescope. An association of recently formed stars is surrounded by the nebula IC 410.

NGC 1931 is a nebula in Auriga, slightly more than one degree to the west of M36. It is considered to be a difficult target for an amateur telescope. NGC 1931 has an approximate integrated magnitude of 10.1;[90] it is 3 by 3 arcminutes. However, it appears to be elongated in an amateur telescope.[109] Some observers may note a green hue in the nebula; a large telescope will easily show the nebula's "peanut" shape, as well as the quartet of stars that are engulfed by the nebula.[84] The open cluster portion of NGC 1931 is classed as a I 3 p n cluster; the nebula portion is classed as both an emission and reflection nebula.[90] NGC 1931 is approximately 6,000 light-years from Earth and could easily be confused with a comet in the eyepiece of a telescope.[110]

NGC 1664 is a fairly large open cluster, with a diameter of 18 arcminutes, and moderately bright, with a magnitude of 7.6, comparable to several other open clusters in Auriga. One open cluster with a similar magnitude is NGC 1778, with a magnitude of 7.7. This small cluster has a diameter of 7 arcminutes and contains 25 stars. NGC 1857, a small cluster, is slightly brighter at magnitude 7.0. It has a diameter of 6 arcminutes and contains 40 stars, making it far more concentrated than the similar-sized NGC 1778. Far dimmer than the other open clusters is NGC 2126 at magnitude 10.2. Despite its dimness, NGC 2126 is as concentrated as NGC 1857, having 40 stars in a diameter of 6 arcminutes.[45]

Meteor showers

The 2007 Aurigid outburst observed from 47,000 feet by a NASA mission.

Auriga is home to two meteor showers. The Aurigids, named for the entire constellation and formerly called the "Alpha Aurigids", are renowned for their intermittent outbursts, such as those in 1935, 1986, 1994, and 2007.[111] They are associated with the comet Kiess (C/1911 N1), discovered in 1911 by Carl Clarence Kiess. The association was discovered after the outburst in 1935 by Cuno Hoffmeister and Arthur Teichgraeber.[112] The Aurigid outburst on September 1, 1935, prompted the investigation of a connection with Comet Kiess, though the 24-year delay between the comet's return caused doubt in the scientific community. However, the outburst in 1986 erased much of this doubt. Istvan Teplickzky, a Hungarian amateur meteor observer, observed many bright meteors radiating from Auriga in a fashion very similar to the confirmed 1935 outburst. Because the position of Teplickzky's observed radiant and the 1935 radiant were close to the position of Comet Kiess, the comet was confirmed as the source of the Aurigid meteor stream.[111]

The Aurigids had a spectacular outburst in 1994, when many

grazing meteors—those that have a shallow angle of entry and seem to rise from the horizon—were observed in California. The meteors were tinted blue and green, moved slowly, and left trails at least 45° long. Because they had such a shallow angle of entry, some 1994 Aurigids lasted up to 2 seconds. Though there were only a few visual observers for part of the outburst, the 1994 Aurigids peak, which lasted less than two hours, was later confirmed by Finnish amateur radio astronomer Ilkka Yrjölä.[111] The connection with Comet Kiess was finally confirmed in 1994.[112] The 2007 outburst of the Aurigids was predicted by Peter Jenniskens and was observed by astronomers worldwide.[113] Despite some predictions that there would be no Alpha Aurigid outburst, many bright meteors were observed throughout the shower, which peaked on September 1 as predicted. Much like in the 1994 outburst, the 2007 Aurigids were very bright and often colored blue and green. The maximum zenithal hourly rate was 100 meteors per hour, observed at 4:15 am, California time (12:15 UTC) by a team of astronomers flying on NASA planes.[114]

The Aurigids are normally a placid Class II meteor shower that peaks in the early morning hours of September 1, beginning on August 28 every year. Though the maximum zenithal hourly rate is 2–5 meteors per hour, the Aurigids are fast, with an entry velocity of 67 kilometres (42 mi)/sec. The annual Aurigids have a radiant located about two degrees north of Theta Aurigae, a third-magnitude star in the center of the constellation.[115] The Aurigids end on September 4.[116] Some years, the maximum rate has reached 9–30 meteors per hour.[113]

The other meteor showers radiating from Auriga are far less prominent and capricious than the Alpha Aurigids. The Zeta Aurigids are a weak shower with a northern and southern branch lasting from December 11 to January 21. The shower peaks on January 1 and has very slow meteors, with a maximum rate of 1–5 meteors per hour. It was discovered by William Denning in 1886 and was discovered to be the source of rare fireballs by Alexander Stewart Herschel.[117] There is another faint stream of meteors called the "Aurigids", unrelated to the September shower. This shower lasts from January 31 to February 23, peaking from February 5 through February 10; its slow meteors peak at a rate of approximately 2 per hour.[118] The Delta Aurigids are a faint shower radiating from Auriga. It was discovered by a group of researchers at New Mexico State University and has a very low peak rate. The Delta Aurigids last from September 22 through October 23, peaking between October 6 and October 15.[119] They may be related to the September Epsilon Perseids, though they are more similar to the Coma Berenicids in that the Delta Aurigids last longer and have a dearth of bright meteors.[120] They too have a hypothesized connection to an unknown short period retrograde comet.[121] The Iota Aurigids are a hypothesized shower occurring in mid-November; its parent body may be the asteroid 2000 NL10, but this connection is highly disputed. The hypothesized Iota Aurigids may instead be a faint stream of Taurids.[122]

See also

References

Citations

  1. ^ Russell 1922, p. 469.
  2. ^ a b c d e f g h Pasachoff 2006.
  3. ^ a b c IAU, The Constellations, Auriga.
  4. ^ Ridpath, Constellations.
  5. ^ Bakich 1995, p. 54.
  6. ^ Bakich 1995, p. 26.
  7. ^ RECONS, The 100 Nearest Star Systems.
  8. ^ Rogers, Mesopotamian Traditions 1998.
  9. ^ Rogers, Mediterranean Traditions 1998.
  10. ^ a b c d e f g h i j k l m n Moore & Tirion 1997, p. 130–131.
  11. ^ a b c d e f g h Ridpath & Tirion 2009, p. 67.
  12. ^ a b c d e Ridpath, Star Tales Auriga.
  13. ^ Krupp 2007.
  14. ^ Staal 1988, p. 79.
  15. ^ Falkner 2011, p. 41.
  16. ^ a b Winterburn 2009, p. 131.
  17. ^ Staal 1988, p. 109.
  18. ^ a b c d e f g h i j k l m n o p q r s t u Ridpath & Tirion 2001, pp. 86–88.
  19. ^ a b Allen 1899, pp. 83–91.
  20. ^ a b Olcott 2004, pp. 65–69.
  21. ^ Staal 1988, p. 29.
  22. ^ OED 2012, agitator, n..
  23. ^ Ridpath, Star Tales Telescopium Herschelii.
  24. ^ Bakich 1995, p. 11.
  25. ^ Pasachoff 2006, pp. 128–129.
  26. ^ Russell 1922, pp. 469–471.
  27. ^ Staal 1988, p. 70.
  28. ^ MacDonald 1998, p. 225.
  29. ^ Aveni 1977, p. 193.
  30. ^ Buckstaff 1927, p. 280.
  31. ^ a b Staal 1988, pp. 221–222.
  32. ^ Goodenough 1953, p. 43.
  33. ^ Goodenough 1953, pp. 26, 43.
  34. ^ Makemson 1941, p. 268.
  35. ^ Makemson 1941, p. 202.
  36. ^ Makemson 1941, p. 252.
  37. ^ Makemson 1941, p. 210.
  38. ^ MacDonald 1998, p. 65.
  39. ^ MacDonald 1998, pp. 44–51.
  40. ^ MacDonald 1998, p. 66.
  41. ^ a b SIMBAD Alpha Aurigae.
  42. ^ a b c d e f g h i j k l m n o p q r s t u v w x y z aa Burnham 1978, pp. 261–296.
  43. ^ a b Davis 1944.
  44. ^ Goodenough 1953, pp. 13–14.
  45. ^ a b c d e f g h i j k l m n o p q r s t u v w x y z aa Moore 2000, pp. 338–340, Table 14.12.
  46. ^ Torres, Claret & Young 2009, p. 1365.
  47. ^ a b SIMBAD Beta Aurigae.
  48. ^ Moore 2000, p. 279.
  49. ^ SIMBAD Beta Tauri.
  50. .
  51. ^ a b SIMBAD Iota Aurigae.
  52. ^ a b c d Kaler 2009.
  53. ^ Kashyap et al. 1994.
  54. ^ a b c d e f Kaler 2008.
  55. ^ a b SIMBAD Delta Aurigae.
  56. ^ Moore 2000, pp. 338–340.
  57. ^ a b SIMBAD Lambda Aurigae.
  58. ^ Hopkins & Stencel 2007.
  59. ^ Hopkins & Stencel 2006.
  60. ^ Lucas, Hopkins & Stencel 2006.
  61. ^ Kaler 2011.
  62. ^ a b SIMBAD Nu Aurigae.
  63. ^ a b SIMBAD Kappa Aurigae.
  64. ^ a b SIMBAD Pi Aurigae.
  65. ^ a b SIMBAD Tau Aurigae.
  66. ^ a b SIMBAD Upsilon Aurigae.
  67. ^ SIMBAD Chi Aurigae.
  68. ^ a b SIMBAD 2 Aurigae.
  69. ^ a b SIMBAD Mu Aurigae.
  70. ^ a b SIMBAD Sigma Aurigae.
  71. ^ a b SIMBAD Omega Aurigae.
  72. ^ a b SIMBAD Xi Aurigae.
  73. ^ a b SIMBAD 9 Aurigae.
  74. ^ SIMBAD Epsilon Aurigae.
  75. ^ a b c SIMBAD Zeta Aurigae.
  76. ^ a b SIMBAD Eta Aurigae.
  77. .
  78. .
  79. ^ a b SIMBAD Psi1 Aurigae.
  80. ^ SIMBAD RT Aurigae.
  81. ^ SIMBAD RX Aurigae.
  82. ^ SIMBAD RW Aurigae.
  83. ^ SIMBAD AE Aurigae.
  84. ^ a b Harrington 1992.
  85. ^ SIMBAD R Aurigae.
  86. ^ SIMBAD UV Aurigae.
  87. ^ SIMBAD U Aurigae.
  88. ^ SIMBAD X Aurigae.
  89. ^ SIMBAD Theta Aurigae.
  90. ^ a b c d e f g h i j k l m n o Thompson & Thompson 2007, pp. 94–101.
  91. ^ Fekel & Tomkin 2007, pp. 59–60.
  92. ^ SIMBAD HR 1528.
  93. ^ .
  94. ^ Exoplanet Encyclopedia HD 40979 b.
  95. .
  96. .
  97. ^ Exoplanet Encyclopedia HD 45350 b.
  98. S2CID 18805775
    .
  99. .
  100. .
  101. ^ Exoplanet Encyclopedia HD 43691 b.
  102. .
  103. ^ Exoplanet Encyclopedia HD 49674 b.
  104. S2CID 17608922
    .
  105. ^ .
  106. ^ Exoplanet Encyclopedia HAT-P-9 b.
  107. ^
    S2CID 119249005
    .
  108. ^ Crossen & Rhemann 2004, p. 177.
  109. ^ a b Higgins 1992.
  110. ^ Levy 2005, pp. 97–99.
  111. ^ a b c Jenniskens 2006, pp. 175–178.
  112. ^ a b Jenniskens 2006, p. 82.
  113. ^ a b Levy 2008, pp. 117–118.
  114. ^ Jenniskens & Kemp 2007.
  115. ^ Lunsford, Activity.
  116. ^ Lunsford, Showers.
  117. ^ Levy 2008, pp. 103–104.
  118. ^ Levy 2008, p. 106.
  119. ^ Levy 2008, p. 119.
  120. ^ Dubietis & Arlt 2002.
  121. ^ Drummond 1982.
  122. ^ Meng 2002.

References

Online sources

SIMBAD

  • "Alpha Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 26 June 2012.
  • "Beta Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 20 August 2012.
  • "Beta Tauri". SIMBAD. Centre de donnés astronomiques de Strasbourg. Retrieved 12 August 2012.
  • "Iota Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 26 June 2012.
  • "Delta Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 27 June 2012.
  • "Lambda Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 26 June 2012.
  • "Nu Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 27 June 2012.
  • "Tau Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 27 June 2012.
  • "Upsilon Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 27 June 2012.
  • "Pi Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 27 June 2012.
  • "Kappa Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 27 June 2012.
  • "Omega Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 27 June 2012.
  • "2 Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 27 June 2012.
  • "9 Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 27 June 2012.
  • "Mu Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 27 June 2012.
  • "Sigma Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 27 June 2012.
  • "Xi Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 27 June 2012.
  • "Epsilon Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 26 June 2012.
  • "Zeta Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 26 June 2012.
  • "Eta Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 26 June 2012.
  • "Psi1 Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 27 June 2012.
  • "Chi Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 20 August 2012.
  • "RT Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 20 August 2012.
  • "RX Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 20 August 2012.
  • "RW Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 20 August 2012.
  • "AE Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 20 August 2012.
  • "R Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 20 August 2012.
  • "UV Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 20 August 2012.
  • "U Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 20 August 2012.
  • "X Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 20 August 2012.
  • "Theta Aurigae". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 27 June 2012.
  • "HR 1528". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 17 July 2012.
  • Roberts, Issac (January 1893). "Nova Aurigæ". Monthly Notices of the Royal Astronomical Society. 53 (3): 123–124. .
  • "Nova Auriga – Evidence in Favour of Impact" (PDF). The Philosophical Institute of Canterbury. A. W. Bickerton. 1 November 1893.
  • "Nova Auriga – Evidence of the Theory of Partile Impact". The Philosophical Institute of Canterbury. Professor A. W. Bickerton. 6 September 1893.
  • Richard A. Gregory (4 May 1893). "Nova Aurigæ – The Genesis of Nova Aruigæ". Nature. 48 (1227): 6–8. .
  • "Beta Tauri (Elnath, El Nath, or Alnath, النطح an-naţħ)". C.D.S. – SIMBAD4 rel 1.197. Retrieved 2012-09-18.

External links