碳星 的英文怎麼說

中文拼音 [tànxīng]
碳星 英文
carbon stars c star
  • 碳 : 名詞[化學] （非金屬元素） carbon （c）
  • 星 : 名詞1 （夜晚天空中閃爍發光的天體） star 2 [天文學] （宇宙間能發射光或反射光的天體） heavenly body...
  1. Usually, carbon stars can be divided into three groups : visual carbon stars, infrared carbon stars and extreme carbon stars

    通常，碳星又主要分為光學碳星、紅外碳星以及極端碳星。
  2. Carbon stars with c / o > 1 are a kind of stars that form at the agb stage and evolved from oxygen - rich agb stars with mid - mass

    碳星是中等質量星演化到agb階段時可能形成的一種恆星，它由氧星演化而來， [ c o ] 1 。
  3. These stars are undergoing important mass loss process and are likely to represent a more evolved phase of the stellar evolution than visual carbon stars

    紅外碳星經歷了重要的質量損失過程，是光學碳星演化的後期。
  4. This present paper is contributed to the study of the evolutionary nature of iso sws spectra from carbon - rich agb stars ( carbon stars ) and molecular and dust features around such carbon stars

    本文主要致力於研究富碳agb星的isosws紅外光譜的演化和它的分子、塵埃特徵。
  5. After competing our work, some conclusions expected are obtained for the evolutionary principles of carbon stars and the evolutionary nature of molecule and dust features around them

    在對它們的研究和分析后得到了我們所期待的關于碳星的一些演化規律和分子、塵埃特徵的演化特性。
  6. By using the iso sws spectra we have studied their physical nature including their molecular and dust features in the circumstellar envelope to make us understand the evolutionary status of carbon stars

    這29顆sic碳星的isosws光譜能很好地反映碳星的演化，有助於我們了解碳星的演化及其分子、塵埃特徵。
  7. The extreme carbon stars, whose derived mass loss rates and optical depths are both very high, are more evolved than infrared carbon stars. these stars are expected to evolve into protoplanatary nebula soon

    極端碳星是高度演化后的紅外碳星，它的質量損失率及光深都非常高，幾乎沒有其光學對應體，並將很快演化為前行星狀星雲。
  8. The infrared carbon stars, whose infrared spectra are mainly due to the dust emission in the circumstellar envelope, are usually believed to be surrounded by the carbon rich envelope characterized by the sic emission feature at 11. 3um

    紅外碳星常被認為有很厚的富碳拱星殼層，它的紅外光譜主要表現為源於拱星殼層的塵埃發射，這個塵埃發射主要以11 . 3 m的sic發射為標記。
  9. We have elected 29 carbon stars with sic emission feature at 11. 3um, i. e. sic carbon stars, which include visual carbon stars, infrared carbon stars and extreme carbon stars to be our working samples in this paper

    本文將選取29顆富碳agb星作為研究對象，它們均有11 . 3 msic發射特徵，在本文中稱之為碳化硅碳星（ sic碳星） ，它們覆蓋了光學碳星、紅外碳星和極端碳星的階段。
  10. Visual carbon stars whose mid - infrared spectra are mainly dominated by photospheric continuum and show large excesses at 60um, represent a transition phase which follows an interruption of mass loss from the oxygen - rich phase and begins a new phase of the mass loss of carbon - rich material. excesses at 60um in these stars are the emission from the residual of oxygen - rich material

    光學碳星的中紅外能量主要來自光球，在60 m處存在超量發射，人們認為其演化階段處在拋射富氧物質終止和新的富碳拱星殼層形成之間，其60 m超量發射就是富氧物質的殘余效應。
  11. Even after making generous assumptions, we determined that the maximum temperature reached in carbonaceous - chondrite asteroids with a diameter of 80 kilometers or more would be only 670 degrees c, too low to cause any melting at all

    即使給予很寬松的假設，我們認為直徑在80公里或以上的碳質球粒隕石小行星，達到的最高溫度只有670 ，不足以造成任何的熔化。
  12. On the other hand, if the mass of the star is greater than about 1. 1 solar masses, the dominate reaction will be the carbon - nitrogen - oxygen cycle

    假若星體質量更大，核聚變便會主要以碳氮氧循環cno循環
  13. Since a carbon nucleus is six times more positively charged than a hydrogen nucleus, the cno cycle can only operate at the higher temperature and density provided by the more massive stars

    但因碳原子核帶的電荷是氫原子核的六倍碳氮氧循環需要只有質量大星體所能提供的較高溫度和壓力才能維持。
  14. Astronomers have known since the 1950s that the chemical element carbon is made in old, red giant stars

    天文學家早在50年代已經知道，碳這種化學元素是在年老的紅巨星內形成。
  15. Composed of micro diamonds, aluminum oxide, and silicon carbide, the isotopic distribution of these grains bore the telltale marks of their birth : ancient supernovas and red giant stars, that shone brightly and then flickered out, billions of years ago, before the birth of the solar system

    由微金剛石、鋁氧化物、碳化硅組成的這些微粒的同位素分佈透露出它們的誕生：那些數十億年前，在太陽系尚未誕生時，曾經閃耀並最終熄滅的古老超新星和紅巨星。
  16. The earth requires greenhouse gases, including water vapor, carbon dioxide and methane, to prevent some of the heat from the received solar radiation from escaping back into space, thus keeping the planet hospitable for protozoa, shetland ponies and lindsay lohan

    地球需要水蒸氣、二氧化碳、甲烷等溫室氣體，把部份的太陽輻射熱能留在大氣層里，好適合原生動物、雪特蘭迷你馬，以及好萊塢女星琳賽蘿涵居住。
  17. Their shells, which apart from hydrogen, helium, and carbon also contain portions of the heavy elements formed in the stellar core, are inherently unstable, and their pulsing creates a withering stellar wind a billion times stronger than the solar wind we know today

    它的殼層除了氫層、氦曾和碳層外還有包含一部分產生自恆星核心的重元素，天生的不穩定，它們的脈動產生了一種毀滅性的星風，比我們現在知道的太陽風要強數百萬倍。
  18. One of these martian meteorites was once thought to harbour signs of life, in the form of carbon - containing compounds and objects that the eye of faith interpreted as fossil bacteria

    這些火星隕石中曾有一個被視作生命的港灣，因為其中含碳化合物和被解釋為細菌化石的物質。
  19. At the end of the process a carbon core of the star will be surrounded by a shell where helium is still being fused into carbon, which in turn is surrounded by and envelope where hydrogen is converted into helium

    該過程結束時碳的星核會被一層仍然在進行氦聚變為碳的殼層包圍，而在這個氦-碳聚變層的外面還包圍著一層由氫-氦聚變層。
  20. Because the photospheric temperature of carbon stars are less than 3000k and the temperature of rich - dust envelope formed by the mass loss is lower, and therefore most of the energy from carbon stars are radiated between 1 to 60um range, in which the vibrational and ro - vibrational bands of many molecules also lies, the study of infrared spectra in this wavelength range is very important to reveal chemical compositions, dust formation process, the atmospheric structure and evolutionary status of stars

    碳星光球的有效溫度不超過3000k ，同時較大的質量損失率形成了富碳的塵埃殼層，以致於它的輻射能量主要集中在1 ? 60 m的紅外波段上，並且許多分子的轉動振動能譜也集中在紅外，因此在紅外波段的研究對揭示碳星化學成份及其分佈、塵埃形成過程、恆星大氣結構和演化狀態都有十分重要的意義。
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