“supernova”的概念、定义、翻译、参考文献-科学参考

supernova

Physics

An explosive brightening of a star in which the energy radiated by it increases by a factor of 10¹⁰. It takes several years to fade, and while it lasts dominates the whole galaxy in which it lies. It is estimated that there could be a supernova explosion in the Milky Way every 30 years, although only six have actually been observed in the last 1000 years. A supernova explosion occurs when a star has burnt up all its available nuclear fuel and the core collapses catastrophically to form a neutron star (see stellar evolution). Supernova explosions are very important, both for creating elements heavier than iron and for dispersing all elements made in stars. Compare nova.

Astronomy

A violent explosion in which certain stars end their lives; given the variable-star type designation SN. In a supernova explosion, the star may become over a billion times brighter than the Sun, and for weeks may outshine the entire galaxy in which it lies. However, the optical luminosity represents only 0.01% of the energy released in the explosion. Most of the energy emerges in the form of neutrinos, and 1% goes into the kinetic energy of the gas expelled. The last supernova seen in our Galaxy was in 1604 (Kepler’s Star), although Supernova 1987A reached naked-eye brightness in the Large Magellanic Cloud. However, two or three supernovae are expected to occur every century in a typical spiral galaxy like ours, which suggests that many have been missed due to absorption of light by dust in the galactic plane.
Supernovae are classified into Types I and II, the latter type showing hydrogen in its spectrum, whereas the spectrum of a Type I supernova shows no hydrogen. There is further subclassification into Types Ia, Ib, and Ic according to other details of the spectrum. Type Ia supernovae reach a maximum magnitude of about −19, while Types Ib and Ic are about 1.5 magnitudes fainter. Type II have a wide range of peak magnitudes, but on average are similar to Types Ib and Ic. Types II, Ib, and Ic occur in young stars of Population I, and thus are concentrated in the disks of spiral galaxies. Type Ia supernovae occur among old stars of Population II, as are found in elliptical galaxies and the halos of spirals.
Type Ia supernovae are believed to be due to the explosion of a white dwarf in a binary as a result of matter falling on to it from its companion star. When the mass of the white dwarf eventually exceeds the Chandrasekhar limit, it undergoes runaway carbon burning and explodes, ejecting about 1 solar mass.
Type Ib and Ic supernovae are thought to result from the collapse of the cores of massive stars which have lost their hydrogen envelopes, either through a stellar wind or by transfer of matter to a companion in a binary. Types Ib and Ic show minor differences in spectra, indicating different compositions of the progenitor stars, which are probably Wolf–Rayet stars stripped of different amounts of their outer layers. Despite their classification, Type Ib and Ic supernovae are more closely related to Type II than to Type Ia.
Type II supernovae arise from the explosion of stars of more than 8 solar masses. Nuclear reactions cease once the star’s core consists of iron and heavier elements, because these elements cannot be burnt to produce energy. The stars then collapse under their own gravity, reaching densities so high that protons and electrons combine to form neutrons, producing a neutron star or even a black hole. The formation of a neutron star causes the overlying layers of material to rebound violently. In this process much of the envelope of the original star, amounting to many solar masses, is ejected at speeds of 2000–20 000 km/s.
Type II supernovae can be subdivided into II-P, II-L, and IIb. Type II-P (for plateau) remain at near-constant brightness for 2–3 months after the outburst before fading. The rarer II-L (for linear) type fades more rapidly from an initial peak. Type IIb show a double maximum in brightness. Type IIb are thought to result from massive stars that have lost most, but not all, of their hydrogen envelope before exploding. The second peak, a few weeks after the initial outburst, is caused by the decay of radioactive nickel and cobalt in the supernova debris. See also supernova remnant.
http://www.cfa.harvard.edu/iau/lists/Supernovae.html Database of all known supernovae, regularly updated.
http://hubblesite.org/image/813/news_release/1999-19

Space Exploration

The explosive death of a star, which temporarily attains a brightness of 100 million Suns or more, so that it can shine as brilliantly as a small galaxy for a few days or weeks. Very approximately, it is thought that a supernova explodes in a large galaxy about once every 100 years. Many supernovae—astronomers estimate around 50%—remain undetected because of obscuration by interstellar dust.
The name ‘supernova’ was coined in 1934 by Swiss astronomer Fritz Zwicky and German-born US astronomer Walter Baade. Zwicky was also responsible for the division of supernovae into types I and II.
Type I supernovae are thought to occur in binary star systems, in which gas from one star falls on to a white dwarf, causing it to explode.
Type II supernovae occur in stars ten or more times as massive as the Sun, which suffer runaway internal nuclear reactions at the ends of their lives, leading to explosions. These are thought to leave behind neutron stars and black holes. Gas ejected by such an explosion causes an expanding radio source, such as the Crab nebula. Supernovae are thought to be the main source of elements heavier than hydrogen and helium.
The first supernova was recorded (although not identified as such at the time) in ad 185 in China. The last supernova was seen in our Galaxy in 1604, but many others have been seen since in other galaxies. In 1987 a supernova visible to the unaided eye occurred in the Large Magellanic Cloud, a small neighbouring galaxy.

单词	supernova
释义	supernova Physics An explosive brightening of a star in which the energy radiated by it increases by a factor of 10¹⁰. It takes several years to fade, and while it lasts dominates the whole galaxy in which it lies. It is estimated that there could be a supernova explosion in the Milky Way every 30 years, although only six have actually been observed in the last 1000 years. A supernova explosion occurs when a star has burnt up all its available nuclear fuel and the core collapses catastrophically to form a neutron star (see stellar evolution). Supernova explosions are very important, both for creating elements heavier than iron and for dispersing all elements made in stars. Compare nova. Astronomy A violent explosion in which certain stars end their lives; given the variable-star type designation SN. In a supernova explosion, the star may become over a billion times brighter than the Sun, and for weeks may outshine the entire galaxy in which it lies. However, the optical luminosity represents only 0.01% of the energy released in the explosion. Most of the energy emerges in the form of neutrinos, and 1% goes into the kinetic energy of the gas expelled. The last supernova seen in our Galaxy was in 1604 (Kepler’s Star), although Supernova 1987A reached naked-eye brightness in the Large Magellanic Cloud. However, two or three supernovae are expected to occur every century in a typical spiral galaxy like ours, which suggests that many have been missed due to absorption of light by dust in the galactic plane. Supernovae are classified into Types I and II, the latter type showing hydrogen in its spectrum, whereas the spectrum of a Type I supernova shows no hydrogen. There is further subclassification into Types Ia, Ib, and Ic according to other details of the spectrum. Type Ia supernovae reach a maximum magnitude of about −19, while Types Ib and Ic are about 1.5 magnitudes fainter. Type II have a wide range of peak magnitudes, but on average are similar to Types Ib and Ic. Types II, Ib, and Ic occur in young stars of Population I, and thus are concentrated in the disks of spiral galaxies. Type Ia supernovae occur among old stars of Population II, as are found in elliptical galaxies and the halos of spirals. Type Ia supernovae are believed to be due to the explosion of a white dwarf in a binary as a result of matter falling on to it from its companion star. When the mass of the white dwarf eventually exceeds the Chandrasekhar limit, it undergoes runaway carbon burning and explodes, ejecting about 1 solar mass. Type Ib and Ic supernovae are thought to result from the collapse of the cores of massive stars which have lost their hydrogen envelopes, either through a stellar wind or by transfer of matter to a companion in a binary. Types Ib and Ic show minor differences in spectra, indicating different compositions of the progenitor stars, which are probably Wolf–Rayet stars stripped of different amounts of their outer layers. Despite their classification, Type Ib and Ic supernovae are more closely related to Type II than to Type Ia. Type II supernovae arise from the explosion of stars of more than 8 solar masses. Nuclear reactions cease once the star’s core consists of iron and heavier elements, because these elements cannot be burnt to produce energy. The stars then collapse under their own gravity, reaching densities so high that protons and electrons combine to form neutrons, producing a neutron star or even a black hole. The formation of a neutron star causes the overlying layers of material to rebound violently. In this process much of the envelope of the original star, amounting to many solar masses, is ejected at speeds of 2000–20 000 km/s. Type II supernovae can be subdivided into II-P, II-L, and IIb. Type II-P (for plateau) remain at near-constant brightness for 2–3 months after the outburst before fading. The rarer II-L (for linear) type fades more rapidly from an initial peak. Type IIb show a double maximum in brightness. Type IIb are thought to result from massive stars that have lost most, but not all, of their hydrogen envelope before exploding. The second peak, a few weeks after the initial outburst, is caused by the decay of radioactive nickel and cobalt in the supernova debris. See also supernova remnant. http://www.cfa.harvard.edu/iau/lists/Supernovae.html Database of all known supernovae, regularly updated. http://hubblesite.org/image/813/news_release/1999-19 Space Exploration The explosive death of a star, which temporarily attains a brightness of 100 million Suns or more, so that it can shine as brilliantly as a small galaxy for a few days or weeks. Very approximately, it is thought that a supernova explodes in a large galaxy about once every 100 years. Many supernovae—astronomers estimate around 50%—remain undetected because of obscuration by interstellar dust. The name ‘supernova’ was coined in 1934 by Swiss astronomer Fritz Zwicky and German-born US astronomer Walter Baade. Zwicky was also responsible for the division of supernovae into types I and II. Type I supernovae are thought to occur in binary star systems, in which gas from one star falls on to a white dwarf, causing it to explode. Type II supernovae occur in stars ten or more times as massive as the Sun, which suffer runaway internal nuclear reactions at the ends of their lives, leading to explosions. These are thought to leave behind neutron stars and black holes. Gas ejected by such an explosion causes an expanding radio source, such as the Crab nebula. Supernovae are thought to be the main source of elements heavier than hydrogen and helium. The first supernova was recorded (although not identified as such at the time) in ad 185 in China. The last supernova was seen in our Galaxy in 1604, but many others have been seen since in other galaxies. In 1987 a supernova visible to the unaided eye occurred in the Large Magellanic Cloud, a small neighbouring galaxy.
随便看	principal formula principal ideal principal ideal domain principal investigator principal moments of inertia principal part principal plane principal point principal principle principal quantum number principal shock principal strain axes principal strain ratio principal value principal value integral principal–agent problem Principia principium individuationis principle of bivalence principle of charity principle of conservation of energy principle of conservation of linear momentum principle of contained fragments principle of contradiction or noncon-tradiction principle of double effect