dwarf star oor Masedonies
dwarf star
en
(astronomy) A star that is located in the main sequence in the Hertzsprung-Russell diagram; fuses hydrogen into helium in its core.
Vertalings in die woordeboek Engels - Masedonies
џуџеста ѕвезда
en
star of relatively small size and low luminosity
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Vertoon algoritmies gegenereerde vertalings
voorbeelde
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In 1932, Landau computed the Chandrashekhar limit; however, he did not apply it to white dwarf stars.
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A mid-sized yellow dwarf star, like the Sun, will remain on the main sequence for about 10 billion years.
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Eddington predicted that dwarf stars remain in an essentially static position on the main sequence for most of their lives.
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HD 134060 is a sun-like yellow dwarf star of spectral type G0VFe+0.4 and magnitude 6.29, around 79 light-years away.
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Lambda Boötis stars are dwarf stars that can be either spectral class A or F. Like BL Boötis-type stars they are metal-poor.
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Type Ia supernova occurs whenever a white dwarf star gains enough additional mass to pass above the Chandrasekhar limit, usually by stealing additional mass from a companion star.
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A white dwarf star in a close binary system can accumulate material from its companion until it ignites and blows off in a thermonuclear explosion, known as a nova.
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A white dwarf star may accumulate sufficient material from a stellar companion to raise its core temperature enough to ignite carbon fusion, at which point it undergoes runaway nuclear fusion, completely disrupting it.
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During his travels to England, Chandrasekhar spent his time working out the statistical mechanics of the degenerate electron gas in white dwarf stars, providing relativistic corrections to Fowler's previous work (see Legacy below).
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At the University of Cambridge, he developed a theoretical model explaining the structure of white dwarf stars that took into account the relativistic variation of mass with the velocities of electrons that comprise their degenerate matter.
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The limit gives the maximum mass of a white dwarf star, ~1.44 solar masses, or equivalently, the minimum mass that must be exceeded for a star to collapse into a neutron star or black hole (following a supernova).
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Contemplation of the diagram led astronomers to speculate that it might demonstrate stellar evolution, the main suggestion being that stars collapsed from red giants to dwarf stars, then moving down along the line of the main sequence in the course of their lifetimes.
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The white dwarf sucks matter from the other star onto an accretion disc and heats up to between 6000 and 10000 K. The dwarf star erupts every 34 to 64 days, reaching magnitude 13.4 in these outbursts and remaining at magnitude 16.8 when quiet.
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Any time two compact objects (white dwarfs, neutron stars, or black holes) are in close orbits, they send out intense gravitational waves.
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A star near the middle of the spectrum, such as the modest Sun or the giant Capella radiates more energy per unit of surface area than the feeble red dwarf stars or the bloated supergiants, but much less than such a white or blue star as Vega or Rigel.
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Yet, it is a remarkable star, dwarfing the planets orbiting it.
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White dwarf – also called a degenerate dwarf, is a small star composed mostly of electron-degenerate matter.
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Also known as Nova Muscae 1983, GQ Muscae is a binary system consisting of a white dwarf and small star that is about 10% as massive as the Sun.
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The system consists of a white dwarf and a donor star which orbit around a common centre of gravity every 97 minutes.
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He was also involved in the early study of brown dwarfs, some of the smallest stars formed.
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Yet even on such scenarios the collisions of UHECRs with white dwarfs and neutron stars would lead to their rapid destruction, but these bodies are observed to be common astronomical objects.
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40 Eridani is a triple star system consisting of an orange main-sequence star, a white dwarf, and a red dwarf.
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The white dwarf accumulates material from its companion star via its accretion disc.
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The central star is a white dwarf of magnitude 14.03.
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AM Canum Venaticorum, a very blue star of magnitude 14, is the prototype of a special class of cataclysmic variable stars, in which the companion star is a white dwarf, rather than a main sequence star.
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72 sinne gevind in 6 ms. Hulle kom uit baie bronne en word nie nagegaan nie.