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LMC195-1
LMC195-1 is a Wolf–Rayet star located in the Large Magellanic Cloud (LMC). It is an extremely rare member of the WO oxygen sequence, at WO2 the hottest known in the LMC. It is likely to be one of the hottest stars known. The star was first observed in a 2013 survey of the Magellanic Clouds using the 1m Swope telescope at Las Campanas Observatory in Chile. The survey was intended to identify Wolf–Rayet candidate stars by taking images through narrow-bandwidth filters centred on the 465.0 nm CIII and 468.6 nm HeII spectral lines together with a continuum filter at 475.0 nm. Digital subtraction of the separate images was used to highlight stars with particularly strong emission at one or both of the indicative spectral lines. The first survey of the Large Magellanic Cloud in October 2013 identified eight previously unknown candidate objects, of which five were later confirmed to be Wolf Rayet stars. LMC 195-1 is located in the rich LH-41 (NGC 1910) stellar associat ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
LH 41-1042
LH 41-1042 is a Wolf–Rayet star located in the Large Magellanic Cloud (LMC). It is an extremely rare member of the WO oxygen sequence, the second to be discovered in the LMC and one of only three found so far in that galaxy. The star was identified in 2012 during an investigation of the LH41 stellar association, also known as NGC 1910, using one of the 6.5m Magellan Telescopes at Las Campanas Observatory in Chile. LH 41-1042 is located in the rich LH 41 (NGC 1910) stellar association that contains two luminous blue variables, S Doradus and R85, the WN5 star BAT99-27, and another WO star LMC195-1. The two WO stars are only 9" apart. WO stars are classified on the basis of OVI emission at 381.1-383.4 nm, which is weak or absent in other Wolf–Rayet stars. The WO4 subclass is defined as having the ratio of OVI to OV emission strength between 0.5 and 1.8. In the new star, the ratio of these line strengths was 0.7. The high temperature and high luminosity of LH 41-1042 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
LH41-1042
LH 41-1042 is a Wolf–Rayet star located in the Large Magellanic Cloud (LMC). It is an extremely rare member of the Wolf–Rayet star, WO oxygen sequence, the second to be discovered in the LMC and one of only three found so far in that galaxy. The star was identified in 2012 during an investigation of the LH41 stellar association, also known as NGC 1910, using one of the 6.5m Magellan Telescopes at Las Campanas Observatory in Chile. LH 41-1042 is located in the rich LH 41 (NGC 1910) stellar association that contains two luminous blue variables, S Doradus and R85, the WN5 star BAT99-27, and another WO star LMC195-1. The two WO stars are only 9" apart. WO stars are classified on the basis of OVI emission at 381.1-383.4 nm, which is weak or absent in other Wolf–Rayet stars. The WO4 subclass is defined as having the ratio of OVI to OV emission strength between 0.5 and 1.8. In the new star, the ratio of these line strengths was 0.7. The high temperature and high luminosi ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
NGC 1910
NGC 1910, or LH-41, is an OB association in the Large Magellanic Cloud. Location NGC 1910's right ascension is and its declination is -69° 14′ 12.1″. Its angular size is 1.54 arcminutes. N119 The cluster has an associated HII region called N119. Stars NGC 1910 contains several stars including S Doradus, LH41-1042, LMC195-1, and R85. Notes References {{DEFAULTSORT:NGC 1910 Dorado (constellation) Open clusters 1910 Events January * January 13 – The first public radio broadcast takes place; live performances of the operas '' Cavalleria rusticana'' and ''Pagliacci'' are sent out over the airwaves, from the Metropolitan Opera House in New York C ... Large Magellanic Cloud ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Wolf–Rayet Star
Wolf–Rayet stars, often abbreviated as WR stars, are a rare heterogeneous set of stars with unusual spectra showing prominent broad emission lines of ionised helium and highly ionised nitrogen or carbon. The spectra indicate very high surface enhancement of heavy elements, depletion of hydrogen, and strong stellar winds. The surface temperatures of known Wolf–Rayet stars range from 20,000 K to around 210,000 K, hotter than almost all other kinds of stars. They were previously called W-type stars referring to their spectral classification. Classic (or population I) Wolf–Rayet stars are evolved, massive stars that have completely lost their outer hydrogen and are fusing helium or heavier elements in the core. A subset of the population I WR stars show hydrogen lines in their spectra and are known as WNh stars; they are young extremely massive stars still fusing hydrogen at the core, with helium and nitrogen exposed at the surface by strong mixing and radia ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
List Of Hottest Stars
This is a list of hottest stars so far discovered (excluding degenerate stars), arranged by decreasing temperature. The stars with temperatures higher than 60,000 K are included. List See also *List of most massive stars *List of most luminous stars *List of least massive stars This is a list of brown dwarfs. These are objects that have masses between heavy gas giants and low-mass stars. The first isolated brown dwarf discovered was Teide 1 in 1995. The first brown dwarf discovered orbiting a star was Gliese 229 B, ... * List of coolest stars References {{Portal bar, Astronomy, Spaceflight, Outer space, Solar System hottest stars, list of Stars, hottest stars, hottest ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
N119
N119 (formally known as LHA 120-N 119) is a spiral-shaped H II region in the Large Magellanic Cloud. Its dimensions are large, at 131 x 175 pc (430 × 570 ly). It contains several luminous stars including S Doradus, LH41-1042, and LMC195-1. Its peculiar S-shaped structure is difficult to explain with classical models. Location With a right ascension of and a declination of , this nebula may be found in the constellation of Dorado about 160 kly (50 kpc) away. Its apparent size is roughly 9′ 14″ × 12′ 15″. It lies at the northern side of the Large Magellanic Cloud's stellar bar, 15′ southeast of the center of rotation of the galaxy's neutral hydrogen. Structure The nebula seems to be in an S-shape, but on closer inspection reveals to have extensions of the spiral arms, ending in a figure 8. The unusual shape may be due to the combination of other nebula, or it may have been formed by perforation of the original molecular cloud by powerful stellar winds and expl ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Wolf–Rayet Stars , which surrounds a Wolf–Rayet star
{{disambiguation ...
Wolf–Rayet (WR) can mean: * Wolf–Rayet star, a type of evolved, massive star * Wolf–Rayet galaxy, which contains large numbers of Wolf–Rayet stars * Wolf–Rayet nebula A Wolf–Rayet nebula is a nebula which surrounds a Wolf–Rayet star. WR nebulae have been classified in various ways. One of the earliest was by the nature and origin of the nebula: * HII regions * ejecta-type nebulae * wind-blown bubbles Th ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Dorado (constellation)
Dorado () is a constellation in the southern sky. It was named in the late 16th century and is now one of the 88 modern constellations. Its name refers to the dolphinfish (''Coryphaena hippurus''), which is known as ''dorado'' in Spanish, although it has also been depicted as a swordfish. Dorado contains most of the Large Magellanic Cloud, the remainder being in the constellation Mensa. The South Ecliptic pole also lies within this constellation. Even though the name Dorado is not Latin but Spanish, astronomers give it the Latin genitive form ''Doradus'' when naming its stars; it is treated (like the adjacent asterism Argo Navis) as a feminine proper name of Greek origin ending in -ō (like ''Io'' or ''Callisto'' or ''Argo''), which have a genitive ending ''-ūs''. History Dorado was one of twelve constellations named by Petrus Plancius from the observations of Pieter Dirkszoon Keyser and Frederick de Houtman. It appeared: * On a celestial globe published in 1597 (or 1598 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Stars In The Large Magellanic Cloud
A star is an astronomical object comprising a luminous spheroid of plasma held together by its gravity. The nearest star to Earth is the Sun. Many other stars are visible to the naked eye at night, but their immense distances from Earth make them appear as fixed points of light. The most prominent stars have been categorised into constellations and asterisms, and many of the brightest stars have proper names. Astronomers have assembled star catalogues that identify the known stars and provide standardized stellar designations. The observable universe contains an estimated to stars. Only about 4,000 of these stars are visible to the naked eye, all within the Milky Way galaxy. A star's life begins with the gravitational collapse of a gaseous nebula of material composed primarily of hydrogen, along with helium and trace amounts of heavier elements. Its total mass is the main factor determining its evolution and eventual fate. A star shines for most of its active life due ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
List Of Most Luminous Stars
This is a list of stars arranged by their absolute magnitude – their intrinsic stellar luminosity. This cannot be observed directly, so instead must be calculated from the apparent magnitude (the brightness as seen from Earth), the distance to each star, and a correction for interstellar extinction. The entries in the list below are further corrected to provide the bolometric magnitude, i.e. integrated over all wavelengths; this relies upon measurements in multiple photometric filters and extrapolation of the stellar spectrum based on the stellar spectral type and/or effective temperature. Entries give the bolometric luminosity in multiples of the luminosity of the Sun () and the bolometric absolute magnitude. As with all magnitude systems in astronomy, the latter scale is logarithmic and inverted i.e. more negative numbers are more luminous. Most stars on this list are not bright enough to be visible to the naked eye from Earth, because of their high distances, high exti ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
List Of Most Massive Stars
This is a list of the most massive stars that have been discovered, in solar masses (). Uncertainties and caveats Most of the masses listed below are contested and, being the subject of current research, remain under review and subject to constant revision of their masses and other characteristics. Indeed, many of the masses listed in the table below are inferred from theory, using difficult measurements of the stars' temperatures and absolute brightnesses. All the masses listed below are uncertain: Both the theory and the measurements are pushing the limits of current knowledge and technology. Both theories and measurements could be incorrect. For example, VV Cephei could be between , or , depending on which property of the star is examined. Complications with distance and obscuring clouds Since massive stars are rare, astronomers must look very far from Earth to find them. All the listed stars are many thousands of light years away, which makes measurements difficult. In addi ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
