Vela constellation lies in the southern hemisphere. Its name means “the sails” in Latin.
Vela was once part of the much larger constellation, Argo Navis, which represented the Argonauts’ ship, but was eventually divided into three smaller constellations: Vela (the sails), Carina (the keel) and Puppis (the stern).
Argo Navis constellation was first catalogued by the Greek astronomer Ptolemy in the 2nd century. The French astronomer Nicolas Louis de Lacaille divided it into three separate constellations in the 1750s.
Vela contains a number of interesting stars and deep sky objects, among them the Eight-burst Nebula (NGC 3132), the Gum Nebula, the Vela Supernova Remnant, the Pencil Nebula (NGC 2736), and the Omicron Velorum Cluster (IC 2391).
FACTS, LOCATION & MAP
Vela is the 32nd constellation in size, occupying an area of 500 square degrees. It is located in the second quadrant of the southern hemisphere (SQ2) and can be seen at latitudes between +30° and -90°. The neighboring constellations are Antlia, Carina, Centaurus, Puppis and Pyxis.
Vela contains five stars with known planets and has no Messier objects. The brightest star in the constellation is Gamma Velorum, with an apparent magnitude of 1.75. There are three meteor showers associated with the constellation: the Delta Velids, the Gamma Velids, and the Puppid-Velids.
Vela represents the sails of the Argo Navis, the ship on which Jason and the Argonauts sailed from Iolcos to get the Golden Fleece. The ship was named after Argus, the shipwright who built it. It was said that the ship was constructed with the help of the goddess Athena. Once the expedition was a success, Argo was consecrated to the sea god Poseidon and then turned into a constellation.
Vela used to be part of the larger Greek constellation Argo Navis along with the constellations Puppis and Carina, which represented the stern and keel of the ship. Argo Navis was divided into the three smaller constellations in 1752 by the French astronomer Nicolas Louis de Lacaille.
Lacaille only used one set of Greek letters for all three constellations, which is why Vela does not have any stars designated Alpha or Beta. The stars that were labelled Alpha and Beta in the constellation Argo Navis now belong to Carina constellation.
MAJOR STARS IN VELA
Suhail – γ Velorum (Gamma Velorum)
Gamma Velorum is the brightest star in Vela constellation. It has an apparent magnitude of 1.7. Gamma Velorum is in fact a multiple star system composed of at least six stars, approximately 336 light years distant from Earth.
The star system’s traditional name, Suhail or Suhail al Muhlif, is derived from the Arabic suhayl al-muħlif, which means “the glorious (star) of the oath.”
The primary component in the system, Gamma-2 Velorum or Gamma Velorum A, is a spectroscopic binary star composed of a blue supergiant with the stellar classification of O7.5 and a massive Wolf-Rayet star, an evolved, extremely hot, massive star which is rapidly losing mass as a result of a very strong stellar wind. The Wolf-Rayet star is one of the nearest supernova candidates to Earth and will likely end its life in a Type Ic supernova explosion. The two stars orbit each other with a period of 78.5 days and are separated by 1 astronomical unit.
The nearest companion to the binary star, Gamma-1 Velorum or Gamma Velorum B, is a blue-white class B subgiant star. Other components of the system are Gamma Velorum C, a white star with a visual magnitude of 8.5, and another binary star composed of Gamma Velorum D and Gamma Velorum E. Gamma Velorum D is another white, class A star with an apparent magnitude of 9.4, and Gamma Velorum E is a 13th magnitude star.
δ Velorum (Delta Velorum)
Delta Velorum is the second brightest star in the constellation. It has an apparent magnitude of 1.96 and is 80.6 light years distant from the Sun. It is located near the border with the constellation Carina.
Delta Velorum is another multiple star system. It is composed of Delta Velorum A and Delta Velorum B, which have a wide orbit and a 142 year orbital period. Delta Velorum A has a visual magnitude of 1.97 and Delta Velorum B has a magnitude of 5.55. The primary component is itself a spectroscopic binary star with an orbital period of 45.15 days. It is the brightest eclipsing binary star system known. Both stars in the system have evolved away from the main sequence. Both are rapid spinners and believed to be about 400 million years old.
Another binary system can be found at a separation of 69 arc seconds. It consists of an 11th magnitude and 13th magnitude stars separated by 6 seconds of arc.
Delta Velorum is sometimes known as Koo She, which is Chinese for “bow and arrows.”
λ Velorum (Lambda Velorum)
Lambda Velorum is the third brightest star in Vela. It has an apparent magnitude of 2.21 and is approximately 545 light years distant from Earth. It shares the traditional name Suhail with the brighter Gamma Velorum. In China, the star is known as Pinyin, which means “judge for estimating the age of animals.”
Lambda Velorum has the stellar classification of K4.5Ib-II, which means that it is an orange star halfway between the bright giant and supergiant stages. It is classified as an LC-type slow irregular variable star. It exhibits variations in brightness ranging from apparent magnitude 2.14 to 2.30.
The star is about 8.5 times more massive than the Sun and 10,000 times more luminous. It is believed to be about 32 million years old. It has a radius 207 times solar.
Markab – κ Velorum (Kappa Velorum)
Kappa Velorum is a spectroscopic binary star approximately 572 light years distant from Earth. It has a visual magnitude of 2.48 and has the combined stellar classification of B2 IV, matching a blue-white subgiant star.
The two stars in the system orbit each other with a period of 116.65 days.
The star has the traditional name Markab (sometimes spelled Markeb to distinguish it from Alpha Pegasi in Pegasus constellation). The name is derived from the Arabic word markab, which means “something to ride.”
μ Velorum (Mu Velorum)
Mu Velorum is another binary star in Vela constellation. It is approximately 117 light years distant from Earth. The two components orbit each other with a period of 116.24 years and are separated by 1.437 seconds of arc. The system has a combined apparent magnitude of 2.69, and the individual stars have visual magnitudes of 2.7 and 6.4.
The brighter component is a yellow giant star with the stellar classification of G5 III. It is about 107 times more luminous than the Sun, has 3.3 times the mass, and 13 times the solar radius. The companion is also a class G (yellow) star, a main sequence dwarf belonging to the stellar class G2V.
N Velorum (HD 82668)
N Velorum is an orange giant star with the stellar classification K5 III. It has an apparent magnitude of 3.16 and is approximately 239 light years distant from the Sun. The star lies on the border between Vela and Carina. It is twice as massive as the Sun and has 29 times the solar radius.
φ Velorum (Phi Velorum)
Phi Velorum is a blue-white supergiant with the stellar classification B5 Ib. It has an apparent magnitude of 3.52 and is approximately 1,590 light years distant from the Sun. The star has the traditional name Tseen Ke, which means “record of heaven” or “star chart” in Chinese.
ο Velorum (Omicron Velorum)
Omicron Velorum is a blue-white subgiant belonging to the stellar class B3 IV. It has an apparent magnitude of 3.60 and is approximately 490 light years distant from the solar system. The star has a mass 5.5 times that of the Sun and a radius 4.3 times solar. It is 1,000 times more luminous than the Sun.
Omicron Velorum is classified as a variable star. Its luminosity varies from magnitude 3.55 to 3.67 over a period of 2.78 days.
ψ Velorum (Psi Velorum)
Psi Velorum is another binary star in Vela. It has an apparent magnitude of 3.60 and is 60.5 light years distant from the Sun. It is the nearest star to Earth located in Vela constellation.
The binary system consists of a yellow-white subgiant with the stellar classification of F3IV and a visual magnitude of 4.1, and a yellow-white main sequence dwarf belonging to the stellar class F0V with an apparent magnitude of 4.6.
The stars orbit each other with a period of 33.99 years and are separated by 0.68 arc seconds.
WISE 1049-5319 is a binary brown dwarf system only 6.6 light years distant from the Sun – the nearest known brown dwarfs to the solar system. It is also the nearest system to the Sun discovered since 1916, when Barnard’s Star was discovered in Ophiuchus constellation.
The primary component has the stellar classification of L8 ± 1. The two stars have an orbital period of about 25 years and orbit each other at a distance of about 3 astronomical units.
The system was discovered by the astronomer Kevin Luhman from Pennsylvania State University, and the discovery was announced on March 11, 2013.
HD 78004 (c Velorum)
HD 78004 is an orange giant star with the stellar classification of K2III. It has an apparent magnitude of 3.75 and an absolute magnitude of -1.14. The star is approximately 309 light years distant from the solar system.
HD 74180 is another binary star in Vela. It has a combined stellar classification of F3Ia and a visual magnitude of 3.77. The primary component in the system is a yellow-white supergiant classified as an irregular variable. Its brightness varies from magnitude 3.77 to 3.91. The companion is a 10th magnitude star separated from the primary by 37.5 arc seconds.
HD 74180 is approximately 3.100 light years distant from Earth.
HD 92139 is a triple star system about 86.5 light years from Earth. It has a combined apparent magnitude of 3.84. The primary component is a yellow-white subgiant with the stellar classification of F3IV and an apparent magnitude of 4.5. It is a spectroscopic binary star with the two components orbiting each other every 10.21 days. The third star in the system is a white main sequence dwarf belonging to the stellar class A6V. The dwarf has a visual magnitude of 5.1 and is separated from the main pair by 0.3 seconds of arc. It orbits the pair with a period of 16.3 years.
HD 75063 is a white giant star belonging to the spectral class A1III. It has a visual magnitude of 3.87 and is approximately 1,550 light years distant from Earth. The star has an absolute magnitude of -4.54.
HD 73526 is a yellow main sequence dwarf belonging to the stellar class G6V. It has an apparent magnitude of 9.00 and is approximately 310 light years distant from the solar system. The star has roughly the same mass as the Sun and 1.49 times the solar radius. It is 1.77 times more luminous than the Sun.
Two planets are known to be orbiting the star. The first one, discovered in 2002, has an orbital period of 187.5 days and the second one, first observed in 2006, completes an orbit around the star every 376.9 days. The planets form a 2:1 resonance: whenever the inner one completes two orbits, the outer one completes one. The inner planet, HD 73526 b, has a mass at least 2.07 times that of Jupiter and the outer one, HD 73526 c, has at least 2.30 Jupiter masses.
WASP-19 is a yellow main sequence dwarf belonging to the stellar class G8V. It has an apparent magnitude of 12.3 and is about 815 light years distant from the Sun.
A hot Jupiter-type planet, WASP-19 b, was discovered orbiting the star in 2009. The planet has the shortest orbital period found so far, only 0.78884 days.
V390 Velorum is an old, massive red giant star with the stellar classification F3e. The star has evolved from the red giant stage and started to throw its hull off, which formed a disk of dust that will eventually form a planetary nebula.
It is about 5,000 times more luminous than the Sun, and approximately 2,600 light years distant from Earth. It has a visual magnitude of 10.48. The star is classified as an RV Tauri type variable. It has a companion that completes an orbit around it every 499 days.
The False Cross
The False Cross is an asterism formed by the stars Delta Velorum, Kappa Velorum, Iota Carinae and Epsilon Carinae in Carina constellation. It was named the False Cross because it is often mistaken for the Southern Cross, which is frequently used in navigation to find true south.
DEEP SKY OBJECTS IN VELA
Eight-Burst Nebula (Southern Ring Nebula) – NGC 3132 (Caldwell 74)
NGC 3132 is a bright planetary nebula in Vela, almost half a light year in diameter. It has an apparent magnitude of 9.87 and is approximately 2,000 light years distant from the Sun. It was named the Eight-Burst Nebula because it appears like the figure 8 in amateur telescopes.
The nebula contains two stars, a 10th magnitude star and a 16th magnitude white dwarf which has blown off its outer layers and whose ultraviolet radiation makes the nebula glow.
Vela Supernova Remnant (Gum 16)
The Vela Supernova Remnant is, as the name says, a supernova remnant in Vela constellation. It has an apparent magnitude of 12 and is approximately 815 light years distant from Earth. It is about 8 degrees in size. The progenitor star is believed to have exploded about 11,000 – 12,300 years ago.
The remnant includes the Pencil Nebula (NGC 2736) and is associated with the Vela Pulsar.
The Vela Supernova Remnant overlaps the Puppis Supernova Remnant in Puppis constellation, which is four times more distant. Both objects are among the brightest, largest X-ray features in the night sky.
In 1998, another supernova was observed in the direction of the Vela remnant, RX J0852.0-4622, approximately 650 light years from Earth.
Vela Pulsar (PSR B0833-45)
The Vela Pulsar is a pulsar associated with the Vela Supernova Remnant. The association, made by astronomers at the University of Sydney in 1968, was evidence that supernovae form neutron stars.
The pulsar is a source of radio, optical, gamma and X-ray emissions. It has an apparent magnitude of 23.6 and is approximately 959 light years distant from the solar system.
The Pencil Nebula – NGC 2736
NGC 2736 is a nebula located near the Vela Pulsar in the Vela Supernova Remnant, approximately 815 light years from Earth. It is believed to have been formed from part of the shock wave of the supernova remnant. It has an apparent magnitude of 12.
The nebula was discovered by the English astronomer John Herschel on March 1, 1835 from the Cape of Good Hope.
Gum Nebula (Gum 12)
The Gum Nebula is an emission nebula spanning about 40 degrees in the constellations Vela and Puppis, about 400 parsecs from Earth.
It contains the Vela Supernova Remnant and is itself believed to be a greatly expanded remnant of a supernova that occurred about a million years ago.
The nebula was discovered by the Australian astronomer Colin Stanley Gum in the 1950s and named after him.
Gum 19 is a star-forming region in Vela, approximately 22,000 light years from Earth. The nebula is illuminated by the large, hot blue supergiant star V391 Velorum. The star has a surface temperature of 30,000 degrees Celsius.
NGC 2670 is an open cluster in Vela. It has an apparent magnitude of 7.8 and is approximately 3,200 light years distant from the Sun. It consists of about 50 moderately bright stars.
NGC 2899 is a planetary nebula about 6,500 light years from Earth. It was discovered by John Herschel in 1835.
NGC 2547 is an open cluster about 1,500 light years from Earth. It has an apparent magnitude of 4.7. It was discovered by Nicolas Louis de Lacaille in 1751 during his expedition to the Cape of Good Hope in South Africa.
The stars in the cluster are believed to be 20 to 35 million years old.
NGC 3201 (Caldwell 79)
NGC 3201 is a globular cluster with a visual magnitude of 8.24. It is about 16,300 light years distant from Earth.
The cluster is about 10.24 billion years old and composed mainly of old stars. It is about 40 light years in radius and dominated by red giants.
NGC 3201 was discovered by the Scottish astronomer James Dunlop on May 28, 1826.
HH 47 (Herbig Haro 47)
HH 47 is a Herbig-Haro object in Vela constellation. It is a patch of nebulosity formed as a result of a young star ejecting narrow jets of gas which then collide with nearby gas and dust clouds.
HH 47 is approximately 1,500 light years distant from Earth.
Omicron Velorum Cluster – IC 2391 (Caldwell 85)
IC 2391 is a young open cluster in Vela, approximately 500 light years from Earth. It has an apparent magnitude of 2.5 and can be seen without binoculars.
The cluster consists of about 30 stars and spans 50 arc minutes.