Canis Major

Last updated

Canis Major
Constellation
Canis Major IAU.svg
List of stars in Canis Major
AbbreviationCMa
Genitive Canis Majoris
Pronunciation /ˌkeɪnɪsˈmeɪdʒər/ KAY-niss MAY-jər, genitive /ˌkeɪnɪsməˈdʒɔːrɪs/ KAY-niss mə-JOR-iss
Symbolismthe greater dog
Right ascension 06h 12.5m to 07h 27.5m [1]
Declination −11.03° to −33.25° [1]
Area 380 sq. deg. (43rd)
Main stars 8
Bayer/Flamsteed
stars		32
Stars with planets 7
Stars brighter than 3.00m5
Stars within 10.00 pc (32.62 ly)1
Brightest star Sirius (α CMa) (−1.46 m )
Messier objects 1
Meteor showers 0
Bordering
constellations
Visible at latitudes between +60° and −90°.
Best visible at 21:00 (9 p.m.) during the month of February.

Canis Major is a constellation in the southern celestial hemisphere. In the second century, it was included in Ptolemy's 48 constellations, and is counted among the 88 modern constellations. Its name is Latin for "greater dog" in contrast to Canis Minor, the "lesser dog"; both figures are commonly represented as following the constellation of Orion the hunter through the sky. The Milky Way passes through Canis Major and several open clusters lie within its borders, most notably M41.

Contents

Canis Major contains Sirius, the brightest star in the night sky, known as the "dog star". It is bright because of its proximity to the Solar System and its intrinsic brightness. In contrast, the other bright stars of the constellation are stars of great distance and high luminosity. At magnitude 1.5, Epsilon Canis Majoris (Adhara) is the second-brightest star of the constellation and the brightest source of extreme ultraviolet radiation in the night sky. Next in brightness are the yellow-white supergiant Delta (Wezen) at 1.8, the blue-white giant Beta (Mirzam) at 2.0, blue-white supergiants Eta (Aludra) at 2.4 and Omicron2 at 3.0, and white spectroscopic binary Zeta (Furud), also at 3.0. The red hypergiant VY CMa is one of the largest stars known, while the neutron star RX J0720.4-3125 has a radius of a mere 5 km.

History and mythology

In western astronomy

In ancient Mesopotamia, Sirius, named KAK.SI.SA2 by the Babylonians, was seen as an arrow aiming towards Orion, while the southern stars of Canis Major and a part of Puppis were viewed as a bow, named BAN in the Three Stars Each tablets, dating to around 1100 BC. In the later compendium of Babylonian astronomy and astrology titled MUL.APIN , the arrow, Sirius, was also linked with the warrior Ninurta, and the bow with Ishtar, daughter of Enlil. [2] Ninurta was linked to the later deity Marduk, who was said to have slain the ocean goddess Tiamat with a great bow, and worshipped as the principal deity in Babylon. [3] The Ancient Greeks replaced the bow and arrow depiction with that of a dog. [4]

Sirius A, the brightest star in the night sky, lies in Canis Major. Sirius 1.jpg
Sirius A, the brightest star in the night sky, lies in Canis Major.

In Greek Mythology, Canis Major represented the dog Laelaps, a gift from Zeus to Europa; or sometimes the hound of Procris, Diana's nymph; or the one given by Aurora to Cephalus, so famed for its speed that Zeus elevated it to the sky. [5] It was also considered to represent one of Orion's hunting dogs, [6] pursuing Lepus the Hare or helping Orion fight Taurus the Bull; and is referred to in this way by Aratos, Homer and Hesiod. The ancient Greeks refer only to one dog, but by Roman times, Canis Minor appears as Orion's second dog. Alternative names include Canis Sequens and Canis Alter. [5] Canis Syrius was the name used in the 1521 Alfonsine tables . [5]

The Roman myth refers to Canis Major as Custos Europae, the dog guarding Europa but failing to prevent her abduction by Jupiter in the form of a bull, and as Janitor Lethaeus , "the watchdog". [7] In medieval Arab astronomy, the constellation became al-Kalb al-Akbar, "the Greater Dog", transcribed as Alcheleb Alachbar by 17th century writer Edmund Chilmead. Islamic scholar Abū Rayḥān al-Bīrūnī referred to Orion as Kalb al-Jabbār, "the Dog of the Giant". [5] Among the Merazig of Tunisia, shepherds note six constellations that mark the passage of the dry, hot season. One of them, called Merzem , includes the stars of Canis Major and Canis Minor and is the herald of two weeks of hot weather. [8]

Canis Major as depicted on the Manuchihr Globe made in Mashhad 1632-33 AD. Adilnor Collection, Sweden. Canis Major on the Manuchihr Globe.jpg
Canis Major as depicted on the Manuchihr Globe made in Mashhad 1632–33 AD. Adilnor Collection, Sweden.

In non-western astronomy

Canis Major, observed above Kuantan (north is towards top right) Canis Major above Kuantan Night Sky.jpg
Canis Major, observed above Kuantan (north is towards top right)

In Chinese astronomy, the modern constellation of Canis Major is located in the Vermilion Bird (南方朱雀; Nán Fāng Zhū Què), where the stars were classified in several separate asterisms of stars. The Military Market (軍市; Jūnshì) was a circular pattern of stars containing Nu3, Beta, Xi1 and Xi2, and some stars from Lepus. [9] The Wild Cockerel (野雞; Yějī) was at the centre of the Military Market, although it is uncertain which stars depicted what. Schlegel reported that the stars Omicron and Pi Canis Majoris might have been them, [10] while Beta or Nu2 have also been proposed. [11] Sirius was Tiānláng (天狼), the Celestial Wolf, [12] denoting invasion and plunder. [11] Southeast of the Wolf was the asterism Húshǐ (弧矢), the celestial Bow and Arrow, which was interpreted as containing Delta, Epsilon, Eta and Kappa Canis Majoris and Delta Velorum. Alternatively, the arrow was depicted by Omicron2 and Eta and aiming at Sirius (the Wolf), while the bow comprised Kappa, Epsilon, Sigma, Delta and 164 Canis Majoris, and Pi and Omicron Puppis. [13]

Both the Māori people and the people of the Tuamotus recognized the figure of Canis Major as a distinct entity, though it was sometimes absorbed into other constellations. Te Huinga-o-Rehua, also called Te Putahi-nui-o-Rehua and Te Kahui-Takurua, ("The Assembly of Rehua" or "The Assembly of Sirius") was a Māori constellation that included both Canis Minor and Canis Major, along with some surrounding stars. [14] [15] Related was Taumata-o-Rehua, also called Pukawanui, the Mirror of Rehua, formed from an undefined group of stars in Canis Major. [16] [17] They called Sirius Rehua and Takarua, corresponding to two of the names for the constellation, though Rehua was a name applied to other stars in various Māori groups and other Polynesian cosmologies. [18] [19] The Tuamotu people called Canis Major Muihanga-hetika-o-Takurua, "the abiding assemblage of Takarua". [20]

The Tharumba people of the Shoalhaven River saw three stars of Canis Major as Wunbula (Bat) and his two wives Murrumbool (Mrs Brown Snake) and Moodtha (Mrs Black Snake); bored of following their husband around, the women try to bury him while he is hunting a wombat down its hole. He spears them and all three are placed in the sky as the constellation Munowra. [21] To the Boorong people of Victoria, Sigma Canis Majoris was Unurgunite (which has become the official name of this star [22] ), and its flanking stars Delta and Epsilon were his two wives. [23] The moon (Mityan, "native cat") sought to lure the further wife (Epsilon) away, but Unurgunite assaulted him and he has been wandering the sky ever since. [24]

Characteristics

Canis Major is a constellation in the Southern Hemisphere's summer (or northern hemisphere's winter) sky, bordered by Monoceros (which lies between it and Canis Minor) to the north, Puppis to the east and southeast, Columba to the southwest, and Lepus to the west. The three-letter abbreviation for the constellation, as adopted by the International Astronomical Union in 1922, is "CMa". [25] The official constellation boundaries, as set by Belgian astronomer Eugène Delporte in 1930, are defined by a quadrilateral; in the equatorial coordinate system, the right ascension coordinates of these borders lie between 06h 12.5m and 07h 27.5m, while the declination coordinates are between −11.03° and −33.25°. [1] Covering 380 square degrees or 0.921% of the sky, it ranks 43rd of the 88 currently-recognized constellations in size. [26]

Features

The stars of Canis Major as they can be seen by the naked eye; lines have been added for clarity. CanisMajorCC.jpg
The stars of Canis Major as they can be seen by the naked eye; lines have been added for clarity.

Stars

Canis Major is a prominent constellation because of its many bright stars. These include Sirius (Alpha Canis Majoris), the brightest star in the night sky, as well as three other stars above magnitude 2.0. [6] Furthermore, two other stars are thought to have previously outshone all others in the night sky—Adhara (Epsilon Canis Majoris) shone at −3.99 around 4.7 million years ago, and Mirzam (Beta Canis Majoris) peaked at −3.65 around 4.42 million years ago. Another, NR Canis Majoris, will be brightest at magnitude −0.88 in about 2.87 million years' time. [27]

The German cartographer Johann Bayer used the Greek letters Alpha through Omicron to label the most prominent stars in the constellation, including three adjacent stars as Nu and two further pairs as Xi and Omicron, [28] while subsequent observers designated further stars in the southern parts of the constellation that were hard to discern from Central Europe. [3] Bayer's countryman Johann Elert Bode later added Sigma, Tau and Omega; [29] the French astronomer Nicolas Louis de Lacaille added lettered stars a to k (though none are in use today). [29] John Flamsteed numbered 31 stars, with 3 Canis Majoris being placed by Lacaille into Columba as Delta Columbae (Flamsteed had not recognised Columba as a distinct constellation). [30] He also labelled two stars—his 10 and 13 Canis Majoris—as Kappa1 and Kappa2 respectively, but subsequent cartographers such as Francis Baily and John Bevis dropped the fainter former star, leaving Kappa2 as the sole Kappa. [28] Flamsteed's listing of Nu1, Nu2, Nu3, Xi1, Xi2, Omicron1 and Omicron2 have all remained in use. [31]

Canis Major as depicted in Urania's Mirror, a set of constellation cards published in London c.1825. Next to it are Lepus and Columba (partly cut off). Sidney Hall - Urania's Mirror - Canis Major, Lepus, Columba Noachi & Cela Sculptoris.jpg
Canis Major as depicted in Urania's Mirror , a set of constellation cards published in London c.1825. Next to it are Lepus and Columba (partly cut off).

Sirius is the brightest star in the night sky at apparent magnitude −1.46 and one of the closest stars to Earth at a distance of 8.6 light-years. Its name comes from the Greek word for "scorching" or "searing". Sirius is also a binary star; its companion Sirius B is a white dwarf with a magnitude of 8.4–10,000 times fainter than Sirius A to observers on Earth. [32] The two orbit each other every 50 years. Their closest approach last occurred in 1993 and they will be at their greatest separation between 2020 and 2025. Sirius was the basis for the ancient Egyptian calendar. [6] The star marked the Great Dog's mouth on Bayer's star atlas. [33]

Flanking Sirius are Beta and Gamma Canis Majoris. Also called Mirzam or Murzim, Beta is a blue-white Beta Cephei variable star of magnitude 2.0, which varies by a few hundredths of a magnitude over a period of six hours. [34] Mirzam is 500 light-years from Earth, and its traditional name means "the announcer", referring to its position as the "announcer" of Sirius, as it rises a few minutes before Sirius does. [6] Gamma, also known as Muliphein, is a fainter star of magnitude 4.12, in reality a blue-white bright giant of spectral type B8IIe located 441 light-years from earth. [35] Iota Canis Majoris, lying between Sirius and Gamma, is another star that has been classified as a Beta Cephei variable, varying from magnitude 4.36 to 4.40 over a period of 1.92 hours. [36] It is a remote blue-white supergiant star of spectral type B3Ib, around 46,000 times as luminous as the sun and, at 2500 light-years distant, 300 times further away than Sirius. [37]

Epsilon, Omicron2, Delta, and Eta Canis Majoris were called Al Adzari "the virgins" in medieval Arabic tradition. [38] Marking the dog's right thigh on Bayer's atlas is Epsilon Canis Majoris, [33] also known as Adhara. At magnitude 1.5, it is the second-brightest star in Canis Major and the 23rd-brightest star in the sky. It is a blue-white supergiant of spectral type B2Iab, around 404 light-years from Earth. [39] This star is one of the brightest known extreme ultraviolet sources in the sky. [40] It is a binary star; the secondary is of magnitude 7.4. Its traditional name means "the virgins", having been transferred from the group of stars to Epsilon alone. [41] Nearby is Delta Canis Majoris, also called Wezen. It is a yellow-white supergiant of spectral type F8Iab and magnitude 1.84, around 1605 light-years from Earth. [42] With a traditional name meaning "the weight", Wezen is 17 times as massive and 50,000 times as luminous as the Sun. If located in the centre of the Solar System, it would extend out to Earth as its diameter is 200 times that of the Sun. Only around 10 million years old, Wezen has stopped fusing hydrogen in its core. Its outer envelope is beginning to expand and cool, and in the next 100,000 years it will become a red supergiant as its core fuses heavier and heavier elements. Once it has a core of iron, it will collapse and explode as a supernova. [43] Nestled between Adhara and Wezen lies Sigma Canis Majoris, known as Unurgunite to the Boorong and Wotjobaluk people, [23] a red supergiant of spectral type K7Ib that varies irregularly between magnitudes 3.43 and 3.51. [44]

Also called Aludra, Eta Canis Majoris is a blue-white supergiant of spectral type B5Ia with a luminosity 176,000 times and diameter around 80 times that of the Sun. [45] Classified as an Alpha Cygni type variable star, Aludra varies in brightness from magnitude 2.38 to 2.48 over a period of 4.7 days. [46] It is located 1120 light-years away. To the west of Adhara lies 3.0-magnitude Zeta Canis Majoris or Furud, around 362 light-years distant from Earth. [47] It is a spectroscopic binary, whose components orbit each other every 1.85 years, the combined spectrum indicating a main star of spectral type B2.5V. [48]

Between these stars and Sirius lie Omicron1, Omicron2, and Pi Canis Majoris. Omicron2 is a massive supergiant star about 21 times as massive as the Sun. [49] Only 7 million years old, [49] it has exhausted the supply of hydrogen at its core and is now processing helium. [50] It is an Alpha Cygni variable that undergoes periodic non-radial pulsations, which cause its brightness to cycle from magnitude 2.93 to 3.08 over a 24.44-day interval. [51] Omicron1 is an orange K-type supergiant of spectral type K2.5Iab that is an irregular variable star, varying between apparent magnitudes 3.78 and 3.99. [52] Around 18 times as massive as the Sun, it shines with 65,000 times its luminosity. [53]

North of Sirius lie Theta and Mu Canis Majoris, Theta being the most northerly star with a Bayer designation in the constellation. [54] Around 8 billion years old, it is an orange giant of spectral type K4III that is around as massive as the Sun but has expanded to 30 times the Sun's diameter. [55] Mu is a multiple star system located around 1244 light-years distant, [56] its components discernible in a small telescope as a 5.3-magnitude yellow-hued and 7.1-magnitude bluish star. [57] The brighter star is a giant of spectral type K2III, [56] while the companion is a main sequence star of spectral type B9.5V. [58] Nu1 Canis Majoris is a yellow-hued giant star of magnitude 5.7, 278 light-years away; it is at the threshold of naked-eye visibility. It has a companion of magnitude 8.1. [6]

At the southern limits of the constellation lie Kappa and Lambda Canis Majoris. Although of similar spectra and nearby each other as viewed from Earth, they are unrelated. [26] Kappa is a Gamma Cassiopeiae variable of spectral type B2Vne, [59] which brightened by 50% between 1963 and 1978, from magnitude 3.96 or so to 3.52. [60] It is around 659 light-years distant. [61] Lambda is a blue-white B-type main sequence dwarf with an apparent magnitude of 4.48 located around 423 light-years from Earth. [62] It is 3.7 times as wide as and 5.5 times as massive as the Sun, and shines with 940 times its luminosity. [54]

Very Large Telescope image of the surroundings of VY Canis Majoris VLT image of the surroundings of VY Canis Majoris seen with SPHERE.jpg
Very Large Telescope image of the surroundings of VY Canis Majoris

Canis Major is also home to many variable stars. EZ Canis Majoris is a Wolf–Rayet star of spectral type WN4 that varies between magnitudes 6.71 and 6.95 over a period of 3.766 days; the cause of its variability is unknown but thought to be related to its stellar wind and rotation. [63] VY Canis Majoris is a remote red hypergiant located approximately 3,800 light-years away from Earth. It is one of largest stars known (sometimes described as the largest known) [64] and is also one of the most luminous with a radius varying from 1,420 to 2,200 times the Sun's radius, and a luminosity around 300,000 times greater than the Sun. Its current mass is about 17 ± 8 solar masses, having shed material from an initial mass of 25–32 solar masses. [65] [66] VY CMa is also surrounded by a red reflection nebula that has been made by the material expelled by the strong stellar winds of its central star. W Canis Majoris is a type of red giant known as a carbon star—a semiregular variable, it ranges between magnitudes 6.27 and 7.09 over a period of 160 days. [67] A cool star, it has a surface temperature of around 2,900 K and a radius 234 times that of the Sun, its distance estimated at 1,444–1,450 light-years from Earth. [68] At the other extreme in size is RX J0720.4-3125, a neutron star with a radius of around 5 km. [69] Exceedingly faint, it has an apparent magnitude of 26.6. [70] Its spectrum and temperature appear to be mysteriously changing over several years. The nature of the changes are unclear, but it is possible they were caused by an event such as the star's absorption of an accretion disc. [69]

Tau Canis Majoris is a Beta Lyrae-type eclipsing multiple star system that varies from magnitude 4.32 to 4.37 over 1.28 days. [71] Its four main component stars are hot O-type stars, with a combined mass 80 times that of the Sun and shining with 500,000 times its luminosity, but little is known of their individual properties. A fifth component, a magnitude 10 star, lies at a distance of 13,000 astronomical units (0.21  ly ). The system is only 5 million years old. [72] UW Canis Majoris is another Beta Lyrae-type star 3000 light-years from Earth; it is an eclipsing binary that ranges in magnitude from a minimum of 5.3 to a maximum of 4.8. It has a period of 4.4 days; [6] its components are two massive hot blue stars, one a blue supergiant of spectral type O7.5–8 Iab, while its companion is a slightly cooler, less evolved and less luminous supergiant of spectral type O9.7Ib. The stars are 200,000 and 63,000 times as luminous as the Sun. However the fainter star is the more massive at 19 solar masses to the primary's 16. [73] R Canis Majoris is another eclipsing binary that varies from magnitude 5.7 to 6.34 over 1.13 days, [74] with a third star orbiting these two every 93 years. The shortness of the orbital period and the low ratio between the two main components make this an unusual Algol-type system. [75]

Seven star systems have been found to have planets. Nu2 Canis Majoris is an ageing orange giant of spectral type K1III of apparent magnitude 3.91 located around 64 light-years distant. [76] Around 1.5 times as massive and 11 times as luminous as the Sun, it is orbited over a period of 763 days by a planet 2.6 times as massive as Jupiter. [77] HD 47536 is likewise an ageing orange giant found to have a planetary system—echoing the fate of the Solar System in a few billion years as the Sun ages and becomes a giant. [78] Conversely, HD 45364 is a star 107 light-years distant that is a little smaller and cooler than the Sun, of spectral type G8V, which has two planets discovered in 2008. With orbital periods of 228 and 342 days, the planets have a 3:2 orbital resonance, which helps stabilise the system. [79] HD 47186 is another sunlike star with two planets; the inner—HD 47186 b—takes four days to complete an orbit and has been classified as a Hot Neptune, while the outer—HD 47186 c—has an eccentric 3.7-year period orbit and has a similar mass to Saturn. [80] HD 43197 is a sunlike star around 183 light-years distant that has two planets: a hot Jupiter-size planet with an eccentric orbit. The other planet, HD 43197 c, is another massive Jovian planet with a slightly oblong orbit outside of its habitable zone. [81]

Z Canis Majoris is a star system a mere 300,000 years old composed of two pre-main-sequence stars—a FU Orionis star and a Herbig Ae/Be star, [82] which has brightened episodically by two magnitudes to magnitude 8 in 1987, 2000, 2004 and 2008. [83] The more massive Herbig Ae/Be star is enveloped in an irregular roughly spherical cocoon of dust that has an inner diameter of 20 AU (3.0×109 km) and outer diameter of 50 AU (7.5×109 km). The cocoon has a hole in it through which light shines that covers an angle of 5 to 10 degrees of its circumference. Both stars are surrounded by a large envelope of in-falling material left over from the original cloud that formed the system. Both stars are emitting jets of material, that of the Herbig Ae/Be star being much larger—11.7 light-years long. [84] Meanwhile, FS Canis Majoris is another star with infra-red emissions indicating a compact shell of dust, but it appears to be a main-sequence star that has absorbed material from a companion. These stars are thought to be significant contributors to interstellar dust. [85]

Deep-sky objects

The band of the Milky Way goes through Canis Major, with only patchy obscurement by interstellar dust clouds. It is bright in the northeastern corner of the constellation, as well as in a triangular area between Adhara, Wezen and Aludra, with many stars visible in binoculars. Canis Major boasts several open clusters. [86] The only Messier object is M41 (NGC 2287), an open cluster with a combined visual magnitude of 4.5, around 2300 light-years from Earth. Located 4 degrees south of Sirius, it contains contrasting blue, yellow and orange stars and covers an area the apparent size of the full moon—in reality around 25 light-years in diameter. [87] Its most luminous stars have already evolved into giants. The brightest is a 6.3-magnitude star of spectral type K3. Located in the field is 12 Canis Majoris, though this star is only 670 light-years distant. [88] NGC 2360, known as Caroline's Cluster after its discoverer Caroline Herschel, is an open cluster located 3.5 degrees west of Muliphein and has a combined apparent magnitude of 7.2. Around 15 light-years in diameter, it is located 3700 light-years away from Earth, [89] and has been dated to around 2.2 billion years old. [90] NGC 2362 is a small, compact open cluster, 5200 light-years from Earth. It contains about 60 stars, of which Tau Canis Majoris is the brightest member. [6] Located around 3 degrees northeast of Wezen, it covers an area around 12 light-years in diameter, though the stars appear huddled around Tau when seen through binoculars. It is a very young open cluster as its member stars are only a few million years old. Lying 2 degrees southwest of NGC 2362 is NGC 2354 a fainter open cluster of magnitude 6.5, with around 15 member stars visible with binoculars. [87] Located around 30' northeast of NGC 2360, [91] NGC 2359 (Thor's Helmet or the Duck Nebula) is a relatively bright emission nebula in Canis Major, with an approximate magnitude of 10, which is 10,000 light-years from Earth. The nebula is shaped by HD 56925, an unstable Wolf–Rayet star embedded within it. [92]

ESO 489-056 is an irregular dwarf galaxy, located 16 million light-years distant. Stars fleeing a cosmic crash.jpg
ESO 489-056 is an irregular dwarf galaxy, located 16 million light-years distant.

In 2003, an overdensity of stars in the region was announced to be the Canis Major Dwarf, the closest satellite galaxy to Earth. However, there remains debate over whether it represents a disrupted dwarf galaxy or in fact a variation in the thin and thick disk and spiral arm populations of the Milky Way. Investigation of the area yielded only ten RR Lyrae variables—consistent with the Milky Way's halo and thick disk populations rather than a separate dwarf spheroidal galaxy. [94] On the other hand, a globular cluster in Puppis, NGC 2298—which appears to be part of the Canis Major dwarf system—is extremely metal-poor, suggesting it did not arise from the Milky Way's thick disk, and instead is of extragalactic origin. [95]

NGC 2207 and IC 2163 are a pair of face-on interacting spiral galaxies located 125 million light-years from Earth. About 40 million years ago, the two galaxies had a close encounter and are now moving farther apart; nevertheless, the smaller IC 2163 will eventually be incorporated into NGC 2207. As the interaction continues, gas and dust will be perturbed, sparking extensive star formation in both galaxies. [96] Supernovae have been observed in NGC 2207 in 1975 (type Ia SN 1975a), [97] 1999 (the type Ib SN 1999ec), [98] 2003 (type 1b supernova SN 2003H), [99] and 2013 (type II supernova SN 2013ai). [100] Located 16 million light-years distant, [93] ESO 489-056 is an irregular dwarf- and low-surface-brightness galaxy that has one of the lowest metallicities known. [101]

Related Research Articles

<span class="mw-page-title-main">Antlia</span> Constellation in the Southern Celestial Hemisphere

Antlia is a constellation in the Southern Celestial Hemisphere. Its name means "pump" in Latin and Greek; it represents an air pump. Originally Antlia Pneumatica, the constellation was established by Nicolas-Louis de Lacaille in the 18th century. Its non-specific (single-word) name, already in limited use, was preferred by John Herschel then welcomed by the astronomic community which officially accepted this. North of stars forming some of the sails of the ship Argo Navis, Antlia is completely visible from latitudes south of 49 degrees north.

<span class="mw-page-title-main">Ara (constellation)</span> Constellation in the southern celestial hemisphere

Ara is a southern constellation between Scorpius, Telescopium, Triangulum Australe, and Norma. It was one of the Greek bulk described by the 2nd-century astronomer Ptolemy, and it remains one of the 88 modern constellations designated by the International Astronomical Union.

<span class="mw-page-title-main">Canis Minor</span> Constellation in the northern celestial hemisphere

Canis Minor is a small constellation in the northern celestial hemisphere. In the second century, it was included as an asterism, or pattern, of two stars in Ptolemy's 48 constellations, and it is counted among the 88 modern constellations. Its name is Latin for "lesser dog", in contrast to Canis Major, the "greater dog"; both figures are commonly represented as following the constellation of Orion the hunter.

<span class="mw-page-title-main">Delphinus</span> Constellation in the northern celestial hemisphere

Delphinus is a small constellation in the Northern Celestial Hemisphere, close to the celestial equator. Its name is the Latin version for the Greek word for dolphin (δελφίς). It is one of the 48 constellations listed by the 2nd century astronomer Ptolemy, and remains one of the 88 modern constellations recognized by the International Astronomical Union. It is one of the smaller constellations, ranked 69th in size. Delphinus' five brightest stars form a distinctive asterism symbolizing a dolphin with four stars representing the body and one the tail. It is bordered by Vulpecula, Sagitta, Aquila, Aquarius, Equuleus and Pegasus.

<span class="mw-page-title-main">Sagitta</span> Constellation in the northern celestial hemisphere

Sagitta is a dim but distinctive constellation in the northern sky. Its name is Latin for 'arrow', not to be confused with the significantly larger constellation Sagittarius 'the archer'. It was included among the 48 constellations listed by the 2nd-century astronomer Ptolemy, and it remains one of the 88 modern constellations defined by the International Astronomical Union. Although it dates to antiquity, Sagitta has no star brighter than 3rd magnitude and has the third-smallest area of any constellation.

<span class="mw-page-title-main">Telescopium</span> Constellation in the southern celestial hemisphere

Telescopium is a minor constellation in the southern celestial hemisphere, one of twelve named in the 18th century by French astronomer Nicolas-Louis de Lacaille and one of several depicting scientific instruments. Its name is a Latinized form of the Greek word for telescope. Telescopium was later much reduced in size by Francis Baily and Benjamin Gould.

<span class="mw-page-title-main">Ursa Minor</span> Constellation in the northern celestial hemisphere

Ursa Minor, also known as the Little Bear, is a constellation located in the far northern sky. As with the Great Bear, the tail of the Little Bear may also be seen as the handle of a ladle, hence the North American name, Little Dipper: seven stars with four in its bowl like its partner the Big Dipper. Ursa Minor was one of the 48 constellations listed by the 2nd-century astronomer Ptolemy, and remains one of the 88 modern constellations. Ursa Minor has traditionally been important for navigation, particularly by mariners, because of Polaris being the north pole star.

<span class="mw-page-title-main">Eta Canis Majoris</span> Star in the constellation Canis Major

Eta Canis Majoris, also named Aludra, is a star in the constellation of Canis Major. Since 1943, the spectrum of this star has served as one of the stable anchor points by which other stars are classified.

<span class="mw-page-title-main">Musca</span> Constellation in the southern celestial hemisphere

Musca is a small constellation in the deep southern sky. It was one of 12 constellations created by Petrus Plancius from the observations of Pieter Dirkszoon Keyser and Frederick de Houtman, and it first appeared on a celestial globe 35 cm (14 in) in diameter published in 1597 in Amsterdam by Plancius and Jodocus Hondius. The first depiction of this constellation in a celestial atlas was in Johann Bayer's Uranometria of 1603. It was also known as Apis for 200 years. Musca remains below the horizon for most Northern Hemisphere observers.

<span class="mw-page-title-main">Aquila (constellation)</span> Constellation near the celestial equator

Aquila is a constellation on the celestial equator. Its name is Latin for 'eagle' and it represents the bird that carried Zeus/Jupiter's thunderbolts in Greek-Roman mythology.

<span class="mw-page-title-main">Beta Canis Majoris</span> Star in the constellation Canis Major

Beta Canis Majoris, also named Mirzam, is a star in the southern constellation of Canis Major, the "Great Dog", located at a distance of about 500 light-years (150 parsecs) from the Sun. In the modern constellation it lies at the position of the dog's front leg.

<span class="mw-page-title-main">Delta Canis Majoris</span> Star in the constellation Canis Major

Delta Canis Majoris, officially named Wezen, is a star in the constellation of Canis Major. It is a yellow-white F-type supergiant with an apparent magnitude of +1.83. Since 1943, the spectrum of this star has served as one of the stable anchor points by which other stars are classified.

<span class="mw-page-title-main">Iota Canis Majoris</span> Variable star in the constellation Canis Major

Iota Canis Majoris, Latinized from ι Canis Majoris, is a solitary variable supergiant star in the southern constellation of Canis Major. It is visible to the naked eye with an apparent visual magnitude that varies between +4.36 and +4.40. The distance to this star is approximately 2,500 light years based on spectroscopic measurements. It is drifting further away with a radial velocity of +42 km/s.

Omicron<sup>2</sup> Canis Majoris Variable star in constellation Canis Major

Omicron2 Canis Majoris is a star in the constellation Canis Major. Since 1943, the spectrum of this star has served as one of the stable anchor points by which other stars are classified. It has an apparent visual magnitude of 3.043, making it one of the brighter members of the constellation. Based upon a distance modulus of 10.2, it is about 3,600 light-years from Earth.

<span class="mw-page-title-main">UW Canis Majoris</span> Beta Lyrae variable star in the constellation Canis Major

UW Canis Majoris is a star in the constellation Canis Major. It is classified as a Beta Lyrae eclipsing contact binary and given the variable star designation UW Canis Majoris. Its brightness varies from magnitude +4.84 to +5.33 with a period of 4.39 days. Bode had initially labelled it as Tau2 Canis Majoris, but this designation had been dropped by Gould and subsequent authors.

<span class="mw-page-title-main">Pi Puppis</span> Second-brightest star in the constellation of Puppis

Pi Puppis, Latinized from π Puppis, also named Ahadi, is the second-brightest star in the southern constellation of Puppis. It has an apparent visual magnitude of 2.733, so it can be viewed with the naked eye at night. Parallax measurements yield an estimated distance of roughly 810 light-years from the Earth. This is a double star with a magnitude 6.86 companion at an angular separation of 0.72 arcsecond and a position angle of 148° from the brighter primary.

<span class="mw-page-title-main">MY Cephei</span> Red supergiant star in the constellation Cepheus

MY Cephei is a red supergiant located in open cluster NGC 7419 in the constellation of Cepheus. It is a semiregular variable star with a maximum brightness of magnitude 14.4 and a minimum of magnitude 15.5.

<span class="mw-page-title-main">VY Canis Majoris</span> Star in the constellation Canis Major

VY Canis Majoris is an extreme oxygen-rich red hypergiant or red supergiant and pulsating variable star 1.2 kiloparsecs from the Solar System in the slightly southern constellation of Canis Major. It is one of the largest known stars, one of the most luminous and massive red supergiants, and one of the most luminous stars in the Milky Way.

<span class="mw-page-title-main">NR Canis Majoris</span> Binary star system in the constellation Canis Major

NR Canis Majoris is a binary star system in the southern constellation of Canis Major, located to the east of Sirius and Gamma Canis Majoris near the constellation border with Puppis. It has a yellow-white hue and is dimly visible to the naked eye with a combined apparent visual magnitude that fluctuates around 5.60. It is located at a distance of approximately 297 light years from the Sun based on parallax. The system is drifting closer to the Sun with a radial velocity of −29 km/s, and in about three million years it is predicted to approach within 14.1+4.7
−4.0 ly. At that time, the star will become the brightest in the night sky, potentially reaching magnitude −0.88.

<span class="mw-page-title-main">Mu Canis Majoris</span> Star in the constellation Canis Major

Mu Canis Majoris is a binary star system in the southern constellation of Canis Major. The pair can be located a little to the southwest of the point midway between Gamma and Theta Canis Majoris, and the components can be split with a small telescope. The system is faintly visible to the naked eye with an apparent visual magnitude of 5.12. Based upon an annual parallax shift of just 2.62 mas as seen from Earth, this system is located roughly 1,200 light years from the Sun.

References

Citations

  1. 1 2 3 "Canis Major, Constellation Boundary". The Constellations. Retrieved 15 November 2012.
  2. ↑ Rogers, John H. (1998). "Origins of the Ancient Constellations: I. The Mesopotamian traditions". Journal of the British Astronomical Association . 108 (1): 9–28. Bibcode:1998JBAA..108....9R.
  3. 1 2 Wagman 2003, p. 71.
  4. ↑ Rogers, John H. (1998). "Origins of the Ancient Constellations: II. The Mediterranean Traditions". Journal of the British Astronomical Association. 108 (2): 79–89. Bibcode:1998JBAA..108...79R.
  5. 1 2 3 4 Allen 1963, p. 117.
  6. 1 2 3 4 5 6 7 Ridpath & Tirion 2001, pp. 98–99.
  7. ↑ Allen 1963, p. 118.
  8. ↑ Oxby, Claire (October 1999). "A Review of African Ethno-Astronomy: With Particular Reference to Saharan Livestock-Keepers". La Ricerca Folklorica (40): 57–58. doi:10.2307/1479768. JSTOR   1479768.
  9. ↑ Schlegel 1967, p. 428.
  10. ↑ Schlegel 1967, p. 430.
  11. 1 2 Ridpath, Ian. "Canis Major – the Greater Dog". Star Tales. Retrieved 1 March 2014.
  12. ↑ Schlegel 1967, p. 431.
  13. ↑ Schlegel 1967, p. 434.
  14. ↑ Makemson 1941, p. 212.
  15. ↑ Makemson 1941, p. 215.
  16. ↑ Makemson 1941, p. 258.
  17. ↑ Makemson 1941, p. 247.
  18. ↑ Makemson 1941, p. 249.
  19. ↑ Makemson 1941, p. 254.
  20. ↑ Makemson 1941, p. 236.
  21. ↑ Ridley, William (1875). Kámilarói, and other Australian languages (PDF) (2nd ed.). Sydney, New South Wales: T. Richards, government printer. pp. 144–45. Archived (PDF) from the original on 2014-03-01.
  22. ↑ "Naming Stars". IAU.org. Retrieved 30 July 2018.
  23. 1 2 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): 220–34. arXiv: 1010.4610 . Bibcode:2010JAHH...13..220H. doi:10.3724/SP.J.1440-2807.2010.03.06. S2CID   118454721.
  24. ↑ Smyth, Robert Brough (1878). The Aborigines of Victoria: with Notes Relating to the Habits of the Natives of other Parts of Australia and Tasmania. Melbourne, Victoria: J. Ferres, government printer. pp.  433–34.
  25. ↑ Russell, Henry Norris (1922). "The New International Symbols for the Constellations". Popular Astronomy . 30: 469–71. Bibcode:1922PA.....30..469R.
  26. 1 2 Bagnall, Philip M. (2012). The Star Atlas Companion: What You Need to Know about the Constellations. New York, New York: Springer. pp. 99–106. ISBN   978-1-4614-0830-7.
  27. ↑ Tomkin, Jocelyn (April 1998). "Once and Future Celestial Kings". Sky and Telescope. 95 (4): 59–63. Bibcode:1998S&T....95d..59T.
  28. 1 2 Wagman 2003, p. 73.
  29. 1 2 Wagman 2003, p. 74.
  30. ↑ Wagman 2003, p. 368.
  31. ↑ Wagman 2003, pp. 73–74.
  32. ↑ Holberg, J.B. (2007). Sirius: Brightest Diamond in the Night Sky. Chichester, United Kingdom: Praxis Publishing. p.  214. ISBN   978-0-387-48941-4.
  33. 1 2 Wagman 2003, p. 504.
  34. ↑ Kaler, James B. (4 May 2007). "Mirzam". Stars. University of Illinois. Retrieved 2 January 2012.
  35. ↑ "Gamma Canis Majoris – Star in Cluster". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 16 February 2014.
  36. ↑ Watson, Christopher (4 January 2010). "Iota Canis Majoris". AAVSO Website. American Association of Variable Star Observers. Retrieved 2 March 2014.
  37. ↑ Kaler, James B. (26 February 2010). "Iota Canis Majoris". Stars. University of Illinois. Retrieved 2 March 2014.
  38. ↑ Knobel, Edward B. (1895). "Al Achsasi Al Mouakket, on a Catalogue of Stars in the Calendarium of". Monthly Notices of the Royal Astronomical Society . 55 (8): 429–38. Bibcode:1895MNRAS..55..429K. doi: 10.1093/mnras/55.8.429 .
  39. ↑ "Epsilon Canis Majoris – Double Star". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 16 February 2014.
  40. ↑ Wilkinson, E.; Green, J.C.; McLean, R.; Welsh, B. (1996). "Extreme Ultraviolet Spectrum of ɛ Canis Majoris Between 600–920 Å". Bull. Am. Astron. Soc. 28 (2): 915. Bibcode:1996BAAS...28..915W.
  41. ↑ 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. p. 23. ISBN   978-1-931559-44-7.
  42. ↑ "Delta Canis Majoris – Variable Star". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 16 February 2014.
  43. ↑ Kaler, James B. "Wezen". Stars website. University of Illinois. Retrieved 17 February 2014.
  44. ↑ Watson, Christopher (4 January 2010). "Sigma Canis Majoris". AAVSO Website. American Association of Variable Star Observers. Retrieved 24 February 2014.
  45. ↑ Jerzykiewicz, M.; Molenda-Zakowicz, J. (2000). "Empirical Luminosities and Radii of Early-Type Stars after Hipparcos" (PDF). Acta Astronomica. 50: 369–80. Bibcode:2000AcA....50..369J. Archived (PDF) from the original on 2019-11-10.
  46. ↑ Watson, Christopher (3 May 2013). "Eta Canis Majoris". AAVSO Website. American Association of Variable Star Observers. Retrieved 5 February 2014.
  47. ↑ "Zeta Canis Majoris – Cepheid Variable". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 17 February 2014.
  48. ↑ Kaler, James B. (2 February 2007). "Furud". Stars website. University of Illinois. Retrieved 17 February 2014.
  49. 1 2 Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (January 2011). "A Catalogue of Young Runaway Hipparcos Stars within 3 kpc from the Sun". Monthly Notices of the Royal Astronomical Society. 410 (1): 190–200. arXiv: 1007.4883 . Bibcode:2011MNRAS.410..190T. doi: 10.1111/j.1365-2966.2010.17434.x . S2CID   118629873.
  50. ↑ Kaler, James B. "Omicron-2 Canis Majoris". Stars. University of Illinois. Retrieved 24 February 2014.
  51. ↑ Lefèvre, L.; Marchenko, S. V.; Moffat, A. F. J.; Acker, A. (November 2009). "A systematic study of variability among OB-stars based on HIPPARCOS photometry". Astronomy and Astrophysics. 507 (2): 1141–1201. Bibcode:2009A&A...507.1141L. doi: 10.1051/0004-6361/200912304 .
  52. ↑ Watson, Christopher (4 January 2010). "Omicron1 Canis Majoris". AAVSO Website. American Association of Variable Star Observers. Retrieved 15 February 2014.
  53. ↑ Kaler, James B. "Omicron1 Canis Majoris". Stars. University of Illinois. Retrieved 24 February 2014.
  54. 1 2 Kaler, James B. (8 March 2013). "Theta Canis Majoris". Stars website. University of Illinois. Retrieved 18 February 2014.
  55. ↑ da Silva, L.; Girardi, L.; Pasquini, L.; Setiawan, J.; von der Lühe, O.; de Medeiros, J.R.; Hatzes, A.; Döllinger, M.P.; Weiss, A. (2006). "Basic Physical Parameters of a Selected Sample of Evolved Stars". Astronomy and Astrophysics. 458 (2): 609–23. arXiv: astro-ph/0608160 . Bibcode:2006A&A...458..609D. doi:10.1051/0004-6361:20065105. S2CID   9341088.
  56. 1 2 "18 Canis Majoris". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 18 February 2014.
  57. ↑ Consolmagno, Guy (2011). Turn Left at Orion: Hundreds of Night Sky Objects to See in a Home Telescope – and How to Find Them. Cambridge, United Kingdom: Cambridge University Press. p. 81. ISBN   978-1-139-50373-0.
  58. ↑ "HD 51251 – Star in double system". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 18 February 2014.
  59. ↑ Watson, Christopher (4 January 2010). "Kappa Canis Majoris". AAVSO Website. American Association of Variable Star Observers. Retrieved 24 February 2014.
  60. ↑ Kaler, James B. (1 March 2013). "Kappa Canis Majoris". Stars. University of Illinois. Archived from the original on 11 February 2017. Retrieved 24 February 2014.
  61. ↑ "Kappa Canis Majoris – Be Star". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 2 March 2014.
  62. ↑ "Lambda Canis Majoris – Star". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 2 March 2014.
  63. ↑ The IUE Mega Campaign: Wind Structure and Variability of HD 50896 (WN5) Astrophysical Journal Letters452 #1, pp. L57 (October 1995) Bibcode : 1995ApJ...452L..57S
  64. ↑ Alcolea, J; Bujarrabal, V; Planesas, P; Teyssier, D; Cernicharo, J; De Beck, E; Decin, L; Dominik, C; Justtanont, K; De Koter, A; Marston, A. P; Melnick, G; Menten, K. M; Neufeld, D. A; Olofsson, H; Schmidt, M; Schöier, F. L; Szczerba, R; Waters, L. B. F. M (2013). "HIFISTARSHerschel/HIFI observations of VY Canis Majoris". Astronomy & Astrophysics. 559: A93. arXiv: 1310.2400 . Bibcode:2013A&A...559A..93A. doi:10.1051/0004-6361/201321683. S2CID   55758451.
  65. ↑ Wittkowski, M.; Hauschildt, P.H.; Arroyo-Torres, B.; Marcaide, J.M. (2012). "Fundamental Properties and Atmospheric Structure of the Red Supergiant VY CMa based on VLTI/AMBER spectro-interferometry". Astronomy & Astrophysics. 540: L12. arXiv: 1203.5194 . Bibcode:2012A&A...540L..12W. doi:10.1051/0004-6361/201219126. S2CID   54044968.
  66. ↑ Kamiński, T; Gottlieb, C. A; Menten, K. M; Patel, N. A; Young, K. H; Brünken, S; Müller, H. S. P; McCarthy, M. C; Winters, J. M; Decin, L (2013). "Pure rotational spectra of TiO and TiO2 in VY Canis Majoris". Astronomy and Astrophysics. 551 (2013): A113. arXiv: 1301.4344 . Bibcode:2013A&A...551A.113K. doi:10.1051/0004-6361/201220290. S2CID   59038056.
  67. ↑ Otero, Sebastian Alberto (7 November 2011). "W Canis Majoris". AAVSO Website. American Association of Variable Star Observers. Retrieved 12 March 2014.
  68. ↑ van Belle, Gerard T.; Paladini, Claudia; Aringer, Bernhard; Hron, Josef; Ciardi, David (2013). "The PTI Carbon Star Angular Size Survey: Effective Temperatures and Non-sphericity". The Astrophysical Journal. 775 (1): 45. arXiv: 1307.6585 . Bibcode:2013ApJ...775...45V. doi:10.1088/0004-637X/775/1/45. S2CID   43847096.
  69. 1 2 Hohle, M.M.; Haberl, F.; Vink, J.; de Vries, C.P.; Turolla, R.; Zane, S.; Méndez, M. (2012). "The Continued Spectral and Temporal Evolution of RX J0720.4-3125". Monthly Notices of the Royal Astronomical Society. 423 (2): 1194–99. arXiv: 1203.3708 . Bibcode:2012MNRAS.423.1194H. doi: 10.1111/j.1365-2966.2012.20946.x . S2CID   55696761.
  70. ↑ Kaplan, D.L.; van Kerkwijk, M.H.; Marshall, H.L.; Jacoby, B.A.; Kulkarni, S. R.; Frail, D.A. (2003). "The Nearby Neutron Star RX J0720.4-3125 from Radio to X-rays". The Astrophysical Journal. 590 (2): 1008–1019. arXiv: astro-ph/0303126 . Bibcode:2003ApJ...590.1008K. doi:10.1086/375052. S2CID   17115753.
  71. ↑ Watson, Christopher (4 January 2010). "Tau Canis Majoris". AAVSO Website. American Association of Variable Star Observers. Retrieved 21 March 2014.
  72. ↑ Kaler, James B. "Tau Canis Majoris". Stars. University of Illinois. Retrieved 22 March 2014.
  73. ↑ Bagnuolo, William G. Jr.; Gies, Douglas R.; Hahula, Michael E.; Wiemker, Rafael; Wiggs, Michael S. (1994). "Tomographic Separation of Composite Spectra. 2: The Components of 29 UW Canis Majoris". The Astrophysical Journal. 423: 446–55. Bibcode:1994ApJ...423..446B. doi: 10.1086/173822 .
  74. ↑ Watson, Christopher (4 January 2010). "R Canis Majoris". AAVSO Website. American Association of Variable Star Observers. Retrieved 18 February 2014.
  75. ↑ Budding, E.; Butland, R. (2011). "Observations and Analysis of the System R Canis Majoris". Monthly Notices of the Royal Astronomical Society. 418 (3): 1764–73. Bibcode:2011MNRAS.418.1764B. doi: 10.1111/j.1365-2966.2011.19597.x .
  76. ↑ "7 Canis Majoris – Variable Star". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 26 February 2014.
  77. ↑ Wittenmyer; Endl, Michael; Wang, Liang; Johnson, John Asher; Tinney, C.G.; O'Toole, S.J. (2011). "The Pan-Pacific Planet Search. I. A Giant Planet Orbiting 7 CMa". Astrophysical Journal . 743 (2): 184–91. arXiv: 1111.1007 . Bibcode:2011ApJ...743..184W. doi:10.1088/0004-637X/743/2/184. S2CID   26948630.
  78. ↑ "Distant World in Peril Discovered from La Silla: Giant Exoplanet Orbits Giant Star". ESO for the Public (Press release). Garching, Germany: European Southern Observatory. 22 January 2003. Retrieved 16 March 2014.
  79. ↑ Correia, A. C. M.; Udry, S.; Mayor, M.; Benz, W.; Bertaux, J.-L.; Bouchy, F.; Laskar, J.; Lovis, C.; Mordasini, C.; Pepe, F.; Queloz, D. (2009). "The HARPS Search for Southern Extra-solar Planets XVI. HD 45364, a Pair of Planets in a 3:2 Mean Motion Resonance". Astronomy and Astrophysics. 496 (2): 521–26. arXiv: 0902.0597 . Bibcode:2009A&A...496..521C. doi:10.1051/0004-6361:200810774. S2CID   119235349.
  80. ↑ Bouchy, François; Mayor, Michel; Lovis, Christophe; Udry, Stéphane; Benz, Willy; Bertaux, Jean-Loup; Delfosse, Xavier; Mordasini, Christoph; Pepe, Francesco; Queloz, Didier; Ségransan, Damien (2009). "The HARPS Search for Southern Extra-solar Planets. XVII. Super-Earth and Neptune-mass Planets in Multiple Planet Systems HD 47186 and HD 181433". Astronomy and Astrophysics. 496 (2): 527–31. arXiv: 0812.1608 . Bibcode:2009A&A...496..527B. doi:10.1051/0004-6361:200810669. S2CID   117778593.
  81. ↑ Naef, Dominique; Mayor, Michel; Lo Curto, Gaspare; Bouchy, François; Lovis, Christophe; Moutou, Claire; Benz, Willy; Pepe, Francesco; Queloz, Didier; Santos, Nuno C.; Ségransan, Damien; Udry, Stéphane; Bonfils, Xavier; Delfosse, Xavier; Forveille, Thierry; Hébrard, Guillaume; Mordasini, Christoph; Perrier, Christian; Boisse, Isabelle; Sosnowska, Danuta (2010). "The HARPS Search for Southern Extrasolar Planets XXIII. 8 Planetary Companions to Low-activity Solar-type Stars". Astronomy and Astrophysics. 523: A15. arXiv: 1008.4600 . Bibcode:2010A&A...523A..15N. doi:10.1051/0004-6361/200913616. S2CID   118845989.
  82. ↑ Szeifert, T.; Hubrig, S.; Schöller, M.; Schütz, O.; Stelzer, B.; Mikulášek, Z. (2010). "The Nature of the Recent Extreme Outburst of the Herbig Be/FU Orionis Binary Z Canis Majoris". Astronomy and Astrophysics. 509: L7. arXiv: 0912.3889 . Bibcode:2010A&A...509L...7S. doi:10.1051/0004-6361/200913704. S2CID   14928968.
  83. ↑ Whelan, E.T.; Dougados, C.; Perrin, M. D.; Bonnefoy, M.; Bains, I.; Redman, M.P.; Ray, T.P.; Bouy, H.; Benisty, M.; Bouvier, J.; Chauvin, G.; Garcia, P.J.V.; Grankvin, K.; Malbet, F. (2010). "The 2008 Outburst in the Young Stellar System Z CMa: The First Detection of Twin Jets". The Astrophysical Journal Letters. 720 (1): L119–24. arXiv: 1008.0111 . Bibcode:2010ApJ...720L.119W. doi:10.1088/2041-8205/720/1/L119. S2CID   119237775.
  84. ↑ Canovas, H.; Min, M.; Jeffers, S.V.; Rodenhuis, M.; Keller, C.U. (2012). "Constraining the Circumbinary envelope of Z Canis Majoris via Imaging Polarimetry". Astronomy & Astrophysics. 543 (A70): 8 pp. arXiv: 1205.3784 . Bibcode:2012A&A...543A..70C. doi:10.1051/0004-6361/201117762. S2CID   53690653.
  85. ↑ Miroshnichenko, Anatoly S. (2007). "Toward Understanding the B[e] Phenomenon. I. Definition of the Galactic FS CMa Stars". The Astrophysical Journal. 667 (1): 497–504. Bibcode:2007ApJ...667..497M. CiteSeerX   10.1.1.548.81 . doi:10.1086/520798. S2CID   40320323.
  86. ↑ Crossen, Craig; Rhemann, Gerald (2004). Sky Vistas: Astronomy for Binoculars and Richest-Field Telescopes. New York, New York: Springer. pp.  113–15. ISBN   978-3-211-00851-5. Canis Major.
  87. 1 2 Kambic, Bojan (2009). Viewing the Constellations with Binoculars: 250+ Wonderful Sky Objects to See and Explore. New York, New York: Springer. pp. 230–32. ISBN   978-0-387-85355-0.
  88. ↑ De Laet, Rony (2011). The Casual Sky Observer's Guide: Stargazing with Binoculars and Small Telescopes. New York, New York: Springer. pp. 95–97. ISBN   978-1-4614-0595-5.
  89. ↑ O'Meara, Stephen James (2002). The Caldwell Objects. Cambridge, United Kingdom: Cambridge University Press. pp. 231–33. ISBN   978-0-521-82796-6.
  90. ↑ Mermilliod, Jean-Claude; Mayor, Michel (1990). "Red Giants in Open Clusters. III - Binarity and Stellar Evolution in Five Intermediate-age Clusters: NGC 2360, 2423, 5822, 6811, and IC 4756". Astronomy and Astrophysics. 273 (1): 61–72. Bibcode:1990A&A...237...61M.
  91. ↑ Thompson, Robert and Barbara (2007). Illustrated Guide to Astronomical Wonders: From Novice to Master Observer. Sebastopol, California: O'Reilly Media, Inc. p. 144. ISBN   978-0-596-52685-6.
  92. ↑ Levy, David H. (2005). Deep Sky Objects. Amherst, New York: Prometheus Books. p.  108. ISBN   978-1-59102-361-6.
  93. 1 2 "Stars Fleeing a Cosmic Crash". ESA/Hubble Picture of the Week. Retrieved 14 August 2013.
  94. ↑ Mateu, Cecilia; Vivas, A. Katherina; Zinn, Robert; Miller, Lissa R.; Abad, Carlos (2009). "No Excess of RR Lyrae Stars in the Canis Major Overdensity". The Astronomical Journal. 37 (5): 4412–23. arXiv: 0903.0376 . Bibcode:2009AJ....137.4412M. doi:10.1088/0004-6256/137/5/4412. S2CID   18967866.
  95. ↑ O'Meara, Stephen James (2011). Deep-Sky Companions: The Secret Deep. Cambridge, United Kingdom: Cambridge University Press. p. 139. ISBN   978-0-521-19876-9.
  96. ↑ Wilkins & Dunn 2006, p. 456.
  97. ↑ Kirshner, Robert P.; Arp, H.C.; Dunlap, J.R. (1976). "Observations of Supernovae – 1975a in NGC 2207 and 1975b in the Perseus Cluster". Astrophysical Journal. 207 (1): 44–52. Bibcode:1976ApJ...207...44K. doi: 10.1086/154465 .
  98. ↑ Jha, S.; Garnavich, P.; Challis, P.; Kirshner, R.; Berlind, P. (1999). "Supernova 1999ec in NGC 2207". IAU Circular. 7269: 2. Bibcode:1999IAUC.7269....2J.
  99. ↑ Bishop, David. "Bright Supernovae – 2003". Rochester University. Retrieved 7 March 2014.
  100. ↑ Alain, Klotz; E., Conseil; M., Fraser; Joseph, Brimacombe; C., Inserra; N., Walton; N., Blagorodnova; M., Nicholl; S., Benetti; A., Pastorello; S., Valenti; S., Taubenberger; J., Smartt S.; K., Smith; D., Young; M., Sullivan; A., Gal-Yam; O., Yaron (2013). "Supernova 2013ai in NGC 2207 = Psn J06161835-2122329". Central Bureau Electronic Telegrams. 3431: 1. Bibcode:2013CBET.3431....1K.
  101. ↑ Kunth, Daniel; Östlin, Goran (2000). "The Most Metal-poor Galaxies". The Astronomy and Astrophysics Review. 10 (1–2): 1–79. arXiv: astro-ph/9911094 . Bibcode:2000A&ARv..10....1K. doi:10.1007/s001590000005. S2CID   15487742.

Bibliography

This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.