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Sh2-264
Sharpless 264, also known as the Lambda Orionis Ring, is a molecular cloud and H II region, which can be seen in the northern region of the Orion molecular cloud complex (OMCC), in the constellation of Orion. The OMCC is one of the best-known star formation regions and the closest sector of the Milky Way to the Solar System where high-mass stars are born. The nebula is named after its main star, λ Orionis, a blue giant responsible for the ionization of the surrounding material.Mathieu, R. D.''The λ Orionis Star Forming Region'' ''in Handbook of Star Forming Regions'', Volume I: The Northern Sky ASP Monograph Publications, vol. 4, Bo Reipurth, December 2008, p. 757, . It is also sometimes called the Angelfish Nebula due to its resemblance as to its lighter areas (pink to peach colour) to an angelfish. In the infrared its ionized boundaries are that which appears, instead. Observations λ Orionis (also known as Meissa or Heka) at about 1,100 light-years is the star representin ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Lambda Orionis
Meissa , designated Lambda Orionis (λ Orionis, abbreviated Lambda Ori, λ Ori) is a star in the constellation of Orion. It is a multiple star approximately away with a combined apparent magnitude of 3.33. The main components are an O8 giant star and a B-class main sequence star, separated by about 4″. Despite Meissa being more luminous and only slightly further away than Rigel, it appears 3 magnitudes dimmer at visual wavelengths, with much of its radiation emitted in the ultraviolet due to its high temperature. Nomenclature ''Lambda Orionis'' is the star's Bayer designation. The traditional name ''Meissa'' derives from the Arabic ''Al-Maisan'' which means 'The Shining One'. ''Al-Maisan'' was originally used for Gamma Geminorum, but was mistakenly applied to Lambda Orionis and the name stuck. In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalog and standardize proper names for stars. The WGSN's first bulle ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Orion Molecular Cloud Complex
The Orion molecular cloud complex (or, simply, the Orion complex) is a star-forming region with stellar ages ranging up to 12 Myr. Two giant molecular clouds are a part of it, Orion A and Orion B. The stars currently forming within the complex are located within these clouds. A number of other somewhat older stars no longer associated with the molecular gas are also part of the complex, most notably the Orion's Belt (Orion OB1b), as well as the dispersed population north of it ( Orion OB1a). Near the head of Orion there is also a population of young stars that is centered on Meissa. The complex is between 1 000 and 1 400 light-years away, and hundreds of light-years across. The Orion complex is one of the most active regions of nearby stellar formation visible in the night sky, and is home to both protoplanetary discs and very young stars. Much of it is bright in infrared wavelengths due to the heat-intensive processes involved in stellar formation, though the complex c ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Barnard 30
Barnard 30 is a dark cloud in the Lambda Orionis ring, north of Lambda Orionis, also called Meissa. The region is about 1300 light years from Earth. The Barnard 30 cloud is one of the regions in the Lambda Orionis Ring where the population of young stars is concentrated, together with the Lambda Orionis cluster and Barnard 35. It contains Herbig-Haro Objects, young stars, brown dwarfs and multiple T Tauri stars. The young population includes HK Orionis, a Herbig Ae/Be star and HI Orionis, a T Tauri star. The stellar population in Barnard 30 is about 2-3 million years old and is therefore significantly younger than the central Lambda Orionis cluster. This cloud is likely shaped by the massive star Meissa and this star is also responsible for triggering star-formation in this cloud. A possible supernova 1 million years ago that possibly has formed the Lambda Orionis ring might be an additional trigger for the star-formation in this region. The region contains a reflection ne ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 34989
HD 34989 is a blue-white star in the main sequence, of apparent magnitude 5.80, in the constellation of Orion (constellation), Orion. It is 1700 Light year, light-years from the Solar System. Observation The star is in the northern celestial hemisphere, but close to the celestial equator; this means that it can be observed from all the inhabited regions of the Earth without difficulty and that it is not visible only in the innermost areas of Antarctica. It appears as circumpolar only far beyond the Arctic polar circle. Its brightness puts it at the limit of visibility to the naked eye, so to be observed without the aid of devices requires a clear, and preferably moonless, sky. The best period for observation in the evening sky is between late October and April from both hemispheres; in February (as at J2000) it is anti-posed from the Sun. In July and August its direction is close to that of the Sun, therefore coinciding with most hours of daylight. Physical chara ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Meissa
Meissa , designated Lambda Orionis (λ Orionis, abbreviated Lambda Ori, λ Ori) is a star in the constellation of Orion. It is a multiple star approximately away with a combined apparent magnitude of 3.33. The main components are an O8 giant star and a B-class main sequence star, separated by about 4″. Despite Meissa being more luminous and only slightly further away than Rigel, it appears 3 magnitudes dimmer at visual wavelengths, with much of its radiation emitted in the ultraviolet due to its high temperature. Nomenclature ''Lambda Orionis'' is the star's Bayer designation. The traditional name ''Meissa'' derives from the Arabic ''Al-Maisan'' which means 'The Shining One'. ''Al-Maisan'' was originally used for Gamma Geminorum, but was mistakenly applied to Lambda Orionis and the name stuck. In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalog and standardize proper names for stars. The WGSN's first bulle ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Collinder 69
The Lambda Orionis Cluster (also known as the Collinder 69) is an open star cluster located north-west of the star Betelgeuse in the constellation of Orion. It is about five million years old and roughly away from the Sun. Included within the cluster is a double star named Meissa. With the rest of Orion, it is visible from the middle of August in the morning sky, to late April before Orion becomes too close to the Sun to be seen well. It can be seen from both the northern hemisphere and the southern hemisphere. Description The cluster is following an orbit through the Milky Way that has a period of 227.4 million years with an ellipticity of 0.06, carrying it as far as from the Galactic Center, and as close as . The inclination of the orbit carries it up to away from the galactic plane. On average it crosses the plane every 33.3 million years. The star cluster is young and contains a large number of low-mass stars, some T Tauri stars and brown dwarfs. One notable member is LO ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Saiph
Saiph , designation Kappa Orionis (κ Orionis, abbreviated Kappa Ori, κ Ori) and 53 Orionis (53 Ori), is the sixth-brightest star in the constellation of Orion. Of the four bright stars that compose Orion's main quadrangle, it is the star at the south-eastern corner. A northern-hemisphere observer facing south would see it at the lower left of Orion, and a southern-hemisphere observer facing north would see it at the upper right. Parallax measurements yield an estimated distance of from the Sun, which is about the same as Betelgeuse. It is smaller, less luminous but hotter at its surface than Rigel with an apparent visual magnitude of 2.1. The luminosity of this star changes slightly, varying by 0.04 magnitudes. Nomenclature ''Kappa Orionis'' is the star's Bayer designation and ''53 Orionis'' its Flamsteed designation. The traditional name ''Saiph'' is from the Arabic ''saif al jabbar'', 'سیف الجبّار' literally '' saif of the giant''. This name was originally ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Barnard 35
Barnard is a version of the surname Bernard, which is a French and West Germanic masculine given name and surname. The surname means as tough as a bear, Bar(Bear)+nard/hard(hardy/tough) __NOTOC__ People Some of the people bearing the surname Barnard in England are thought to have arrived after the time of the Norman Conquest (1066), Changing their surnames from Bernard to Barnard. Some of whom, it has been suggested, can be traced back to Hugo Bernard. Some of the Barnard family in England may have been Huguenots who fled from the Atlantic coast region of France ''circa'' 1685 (the time of the revocation of the edict of Nantes) or earlier than that date. By contrast, the Barnard family in Holland (the western provinces of the Netherlands) can be definitively traced back to ''circa'' 1751 (Izaak Barnard) of Scheveningen.The surname Barnard is also found in South Africa among the Afrikaner community. An example of this is Christiaan Barnard, A South African Cardiac Surg ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Spitzer Space Telescope
The Spitzer Space Telescope, formerly the Space Infrared Telescope Facility (SIRTF), was an infrared space telescope launched in 2003. Operations ended on 30 January 2020. Spitzer was the third space telescope dedicated to infrared astronomy, following IRAS (1983) and ISO (1995–1998). It was the first spacecraft to use an Earth-trailing orbit, later used by the Kepler planet-finder. The planned mission period was to be 2.5 years with a pre-launch expectation that the mission could extend to five or slightly more years until the onboard liquid helium supply was exhausted. This occurred on 15 May 2009. Without liquid helium to cool the telescope to the very low temperatures needed to operate, most of the instruments were no longer usable. However, the two shortest-wavelength modules of the IRAC camera continued to operate with the same sensitivity as before the helium was exhausted, and continued to be used into early 2020 in the Spitzer Warm Mission. During the warm mission, t ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Blue-white Main Sequence Star
In astronomy, stellar classification is the classification of stars based on their spectral characteristics. Electromagnetic radiation from the star is analyzed by splitting it with a prism or diffraction grating into a spectrum exhibiting the rainbow of colors interspersed with spectral lines. Each line indicates a particular chemical element or molecule, with the line strength indicating the abundance of that element. The strengths of the different spectral lines vary mainly due to the temperature of the photosphere, although in some cases there are true abundance differences. The ''spectral class'' of a star is a short code primarily summarizing the ionization state, giving an objective measure of the photosphere's temperature. Most stars are currently classified under the Morgan–Keenan (MK) system using the letters ''O'', ''B'', ''A'', ''F'', ''G'', ''K'', and ''M'', a sequence from the hottest (''O'' type) to the coolest (''M'' type). Each letter class is then subdivide ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Phi2 Orionis
Phi2 Orionis is a star in the constellation Orion, where it forms a small triangle on the celestial sphere with the nearby Meissa and Phi1 Orionis. This star is visible to the naked eye with an apparent visual magnitude of 4.081. Based upon an annual parallax shift of 27.76 mas, it is located around 117 light-years from the Sun. This is a G-type giant or subgiant star with a stellar classification of G8 III-IV that, at the age of 6.9 billion years, is evolving away from the main sequence. It has 1.07 times the mass of the Sun, but has expanded to 7.72 times the Sun's radius. The star shines with 31.6 times the solar luminosity from its outer atmosphere at an effective temperature of . References {{DEFAULTSORT:Phi2 Orionis G-type giants Orionis, Phi Orion (constellation) Durchmusterung objects Orionis, 40 037160 026366 1907 Events January * January 14 – 1907 Kingston earthquake: A 6.5 Mw earthquake in Kingston, Jamai ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Orange Giant
A giant star is a star with substantially larger radius and luminosity than a main-sequence (or ''dwarf'') star of the same surface temperature.Giant star, entry in ''Astronomy Encyclopedia'', ed. Patrick Moore, New York: Oxford University Press, 2002. . They lie above the main sequence (luminosity class V in the Yerkes spectral classification) on the Hertzsprung–Russell diagram and correspond to luminosity classes II and III.giant, entry in ''The Facts on File Dictionary of Astronomy'', ed. John Daintith and William Gould, New York: Facts On File, Inc., 5th ed., 2006. . The terms ''giant'' and ''dwarf'' were coined for stars of quite different luminosity despite similar temperature or spectral type by Ejnar Hertzsprung about 1905. Giant stars have radii up to a few hundred times the Sun and luminosities between 10 and a few thousand times that of the Sun. Stars still more luminous than giants are referred to as supergiants and hypergiants. A hot, luminous main-sequence st ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
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