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O-type Main-sequence Star
An O-type main-sequence star (O V) is a main-sequence (core hydrogen-burning) star of spectral type O and luminosity class V. These stars have between 15 and 90 times the mass of the Sun and surface temperatures between 30,000 and 50,000 K. They are between 40,000 and 1,000,000 times as luminous as the Sun. Spectral standard stars The "anchor" standards which define the MK classification grid for O-type main-sequence stars, i.e. those standards which have not changed since the early 20th century, are (O7 V) and (O9 V). The Morgan–Keenan–Kellerman (MKK) "Yerkes" atlas from 1943 listed O-type standards between O5 and O9, but only split luminosity classes for the O9s. The two MKK O9 V standards were Iota Orionis and . The revised Yerkes standards ("MK") presented listed in Johnson & Morgan (1953) presented no changes to the O5 to O8 types, and listed 5 O9 V standards (, , , , 10 Lacertae) and 3 O9.5 V standards (, Sigma Orionis, Zeta ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
O-type Star
An O-type star is a hot, blue star of spectral type O in the Yerkes classification system employed by astronomers. They have surface temperatures in excess of 30,000 kelvins (K). Stars of this type have strong absorption lines of ionised helium, strong lines of other ionised elements, and hydrogen and neutral helium lines weaker than spectral type B. Stars of this type are very rare, but because they are very bright, they can be seen at great distances; out of the 90 brightest stars as seen from Earth, 4 are type O. Due to their high mass, O-type stars end their lives rather quickly in violent supernova explosions, resulting in black holes or neutron stars. Most of these stars are young massive main sequence, giant, or supergiant stars, but also some central stars of planetary nebulae, old low-mass stars near the end of their lives, which typically have O-like spectra. O-type stars are typically found in regions of active star formation, such as the s ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Iota Orionis
Iota Orionis (ι Orionis, abbreviated ι Ori) is a Star system, multiple star system in the celestial equator, equatorial constellation of Orion (constellation), Orion the hunter. It is the eighth-brightest member of Orion with an Apparent magnitude, apparent visual magnitude of 2.77 and also the brightest member of the Asterism (astronomy), asterism known as Orion's Sword. It is a member of the NGC 1980 open cluster. From parallax measurements, it is located at a distance of roughly from the Sun. The system has three visible components designated Iota Orionis A, B and C. Iota Orionis A has also been resolved using speckle interferometry and is also a massive Binary star#Spectroscopic binaries, spectroscopic binary, with components Iota Orionis Aa1 (officially named Hatysa ), Aa2, and Ab. Nomenclature ''ι Orionis'' (Latinisation of names, Latinised to ''Iota Orionis'') is the system's Bayer designation. The designations of the three constituents as ''Iota Orionis ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
BI 253
BI 253 is an O2V star in the Large Magellanic Cloud and is a primary standard of the O2 type. It is one of the hottest main-sequence stars known and one of the most-massive and most-luminous stars known. Discovery BI 253 was first catalogued in 1975 as the 253rd of 272 likely O and early B stars in the Large Magellanic Cloud. In 1995, the spectral type was analysed to be O3 V, the earliest type defined at that time. When the classification of the earliest type O stars was refined in 2002, the complete lack of neutral helium or doubly ionised nitrogen lines in the spectrum led to BI 253 being placed in a new O2 V class. It was given a ((f*)) qualifier because of the very weak emission lines of helium and nitrogen. The most recent published data gives a spectral type of O2V-III(n)((f*)), although it is unclear whether this is due to higher quality spectra or an actual change in the spectrum. BI 253 has been identified as a runaway star because of its relatively iso ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HDE 303308
HDE may refer to: * Hedge End railway station, in England * Henry Draper Extension, an astronomical catalogue * High dose estrogen, a hormonal therapy * Higher Diploma in Education * Home Defence Executive The Home Defence Executive (H.D.E.) was formed on 10 May 1940 under General Sir Edmund Ironside, Commander-in-chief Home Forces, to organise the defence of Britain from invasion by the Axis powers Collier, Basil. "The defence of the United Kingdo ... * Humanitarian Device Exemption * German Trade Association {{disambiguation ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 46149
HD may refer to: Business * H-D or Harley-Davidson, a motorcycle manufacturer * The Home Depot, NYSE stock symbol: HD Chemistry * Hydrogen deuteride, a diatomic compound of hydrogen and deuterium * Mustard gas Codes * Air Do, formerly Hokkaido International Airlines, IATA designator * HD postcode area, covering Huddersfield, Brighouse and Holmfirth in England, UK * Heidelberg's vehicle registration plate code * Hunedoara County (Romania)'s ISO 3166 code Medicine * Hansen's disease or leprosy * Hirschsprung's disease, a disorder of the abdomen * Huntington's disease, a genetic disorder affecting the central nervous system ** HD (gene) or huntingtin, the IT15 gene, which codes for the huntingtin protein People * H.D. or Hilda Doolittle (1886–1961), American poet and novelist Other uses * ''Helsingborgs Dagblad'', a Swedish newspaper * Henry Draper Catalogue, an astronomical catalogue often used to designate stars * Department of Highways (other) * ' ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 46150
NGC 2244 (also known as Caldwell 50 or the Satellite Cluster) is an open cluster in the Rosette Nebula, which is located in the constellation Monoceros. This cluster has several O-type stars, super hot stars that generate large amounts of radiation and stellar wind. The age of this cluster has been estimated to be less than 5 million years. The brightest star in the direction of the cluster is 12 Monocerotis, a foreground K-class giant. The two brightest members of the cluster are HD 46223 of spectral class O4V, 400,000 times brighter than the Sun, and approximately 50 times more massive, and HD 46150, whose spectral type is O5V, has a luminosity 450,000 time larger than that of our star, and is up to 60 times more massive, but it may actually be a double star.A quantitative study of O stars in NGC 2244 and the Monoceros OB2 association, Martins, F.; Mahy, L.; Hillier, D. J.; Rauw, G., ''Astronomy and Astrophysics'' 538, pp. A39, , . These stars do not seem to pulsate, which is ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Zeta Ophiuchi
Zeta Ophiuchi (ζ Oph, ζ Ophiuchi) is a single star located in the constellation of Ophiuchus. It has an apparent visual magnitude of 2.6, making it the third-brightest star in the constellation. Parallax measurements give an estimated distance of roughly from the Earth. It is surrounded by the Sh2-27 nebula, the star's bow shock as it ploughs through dense dust clouds near the Rho Ophiuchi cloud complex. In April 2010, ζ Ophiuchi was occulted by asteroid 824 Anastasia. Properties ζ Ophiuchi is an enormous star with more than 20 times the Sun's mass and eight times its radius. The stellar classification of this star is O9.5 V, with the luminosity class of V indicating that it is generating energy in its core by the nuclear fusion of hydrogen. From Earth, the apparent effective temperature of the star appears to be 34,300K, giving the star the blue hue of an O-type star. However, since the star is rapidly rotating, the exact surface temperature varies across the surf ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Sigma Orionis
Sigma Orionis or Sigma Ori (σ Orionis, σ Ori) is a multiple star system in the constellation Orion (constellation), Orion, consisting of the brightest members of a young open cluster. It is found at the eastern end of Orion's Belt, the belt, south west of Alnitak and west of the Horsehead Nebula which it partially illuminates. The combined brightness of the component stars is magnitude 3.80. History σ Orionis is a naked eye star at the eastern end of Orion's Belt, and has been known since antiquity, but it was not included in Ptolemy's Almagest. It was referred to by Al Sufi, but not formally listed in his catalogue. In more modern times, it was measured by Tycho Brahe and included in his catalogue. In Kepler's extension it is described as "Quae ultimam baltei praecedit ad austr." (preceding the outermost of the belt, to the south). It was then recorded by Johann Bayer in his Uranometria as a single star with the Greek letter σ (sigma). He described i ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 34078
AE Aurigae (abbreviated as AE Aur) is a runaway star in the constellation Auriga; it lights the Flaming Star Nebula. Description AE Aurigae is a blue O-type main sequence star with a mean apparent magnitude of +6.0, making it faintly visible to the naked eye under very good observing conditions. It was discovered to be a variable star by Daniel Walter Morehouse, in 1923, and received its variable star designation in 1924. It is classified as an Orion type variable star and its brightness varies irregularly between magnitudes +5.78 and +6.08. It is approximately 1,300 light-years from Earth. It is a runaway star that might have been ejected during a collision of two binary star groups. This collision, which also is credited with ejecting Mu Columbae and possibly 53 Arietis, has been traced to the Trapezium cluster in the Orion Nebula two million years ago. The binary Iota Orionis may have been the other half of this collision. AE Aur is seen to light up the F ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
14 Cephei
LZ Cephei, also known by its Flamsteed designation 14 Cephei, is a star about 3,600 light years from the Earth, in the constellation Cepheus. Its apparent magnitude is 5.6, making it faintly visible to the naked eye of an observer far from city lights. The star is a rotating ellipsoidal variable whose brightness, as measured by the ''Hipparcos'' satellite, varies between magnitude 5.52 and 5.61. LZ Cephei was discovered to be a binary star by William Edmund Harper in 1931. The orbital elements were first calculated by Robert Methven Petrie in 1962. It was discovered to be a variable star in 1972 by N. Kameswara Rao, using the Lick Observatory's 24 inch telescope. The star was given the variable star designation LZ Cephei in 1973. It was classified as an ellipsoidal variable by Hill ''et al.'' in 1976. A 2011 study of LZ Cephei concluded that the existing data are best explained if the system is a semi-detached binary with either the primary or secondary star nearly ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
