恆星質量 的英文怎麼說

中文拼音 [héngxīngzhíliáng]
恆星質量 英文
stellar mass
  • 恆 : Ⅰ形容詞1 （永久; 持久） permanent; lasting 2 （平常; 經常） usual; common; constant Ⅱ名詞1 （恆心...
  • 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...
  • 質 : Ⅰ名詞1 （性質; 本質） nature; character; essence 2 （質量） quality 3 （物質） matter; substance;...
  • 量 : 量動1. （度量） measure 2. （估量） estimate; size up
  • 恆星 : [天文學] fixed star; star恆星大氣 stellar atmosphere; 恆星導航 star navigation; stellar guidance;...
  • 質量 : 1 [物理學] mass 2 （產品或工作的優劣程度） quality 3 economy （離子源的）; 質量標準 quality level...
  1. As the accretion disk feeds more mass into itself, the embryo star contracts, growing ever denser and more massive.

    隨著吸積盤獲得越來越多的物質，胚胎恆星就不斷收縮，密度和質量都變得越來越大。
  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. Because of gravitational attraction, the escape velocity at the surface of a star, say, will be higher if the star is smaller in size or heavier

    恆星質量越大，體積越小，引力的羈絆便越大，所需逃逸速度亦越高。
  4. A quantitative analysis of this idea led to the prediction that a star remaining about three times the mass of the sun at the end of its evolution ( usually as a neutron star ), will almost inevitably shrink to the critical size needed to undergo a gravitational collapse

    該想法的定量分析導致預言一顆恆星在終止它演化時候保持大約三倍太陽的質量（通常看做一顆中子星） ，將會幾乎不可避免收縮到臨界體積必須遭受引力坍塌。
  5. Evolution of stars of all masses takes place on a hydrodynamic time scale.

    各種質量的恆星的演化，均以流體力學的時間尺度進行。
  6. Previously, only the supermassive black hole there was thought to be able to produce these " hypervelocity " stars

    先前僅僅只認為超大質量黑洞才能製造這些高速恆星。
  7. On the bases of the galaxy evolution theory, we use the therotical chemical evolution model of three zone ( such as halo, thick disk and thin isk ) and multi - phase ( diffuse gas, molecular clouds, stars of both low and high mass, the remnants ). by comparing with the observational constraints, such assurface densities, age - metallicity relation, g - dwarf metallicity distribution in the solar neighbourhood and the correlation between [ a / fe ] and [ fe / h ], supernovae rates, infall rates. the rationality of the model is verified. based on the theory model, we calculate the abundance of neutron capture element

    本文正是在銀河系化學演化的基礎上，利用銀河系的三成分（ threezone ） （即暈、厚盤和薄盤）多相（ multi - phase ） （氣體，分子云，大、小質量恆星以及剩餘物質）的化學演化的理論模型，通過與觀測約束（質量面密度、場星的年齡-金屬豐度關系、太陽附近g矮星金屬含量分佈函數、三成份的特徵量、元素的星系化學演化、超新星的爆炸率、內落速率等）的比較，來檢驗模型的合理性。
  8. Astronomers tacitly assume that stars of the same luminosity and color all have the same mass.

    天文學家心照不宣地默認，光度和顏色都相同的恆星具有相同的質量。
  9. In this situation astronomers tacitly assume that stars of the same luminosity and color all have the same mass.

    在目前的狀況下，天文學家心照不宣地默認，光度和顏色都相同的恆星具有相同的質量。
  10. Massive stars are hottest in their central regions.

    大質量恆星的中心區域溫度最高。
  11. Which is very dim and hence very difficult to find. if it is massive enough though model dependent, the lower mass limit is about 0. 1 solar mass, the gas in the protostar continues to heat up until the central portion becomes hot and dense enough for, say, the hydrogen nuclei to overcome their mutual electrical repulsion. nuclear fusion will then take place and a star is finally born

    如果原行星質量足夠大下限約為0 . 1個太陽質量，要注意的是，不同的理論模型會給出不同的下限，原恆星會不斷變熱，直至核心部分足夠熱和高壓，令氫原子核克服質子間的電排斥力，產生核聚變，成為一顆真正的恆星。
  12. The luminosity per surface area will increase because the temperature increases. but if a star is not very massive, its luminosity will drop because the size of the star protostar decreases much faster

    每單位面積的光度會隨著恆星的溫度增加而上升，但假若恆星原恆星質量不足，它的光度會由於星體體積下降過速而不升反減。
  13. One solar mass is defined to be the mass of our sun, which is about 2x10

    以太陽的質量為比較標準，是天文學家常用的恆星質量單位大約等於2x10
  14. If that happens before the embryo has had time to attain stellar mass, the result is a brown dwarf

    假如這發生在胚胎達到恆星質量之前，結果就是一顆棕矮星。
  15. The first is stellar - mass black holes, having a mass of a few solar masses as the name indicates. they are the end products of stellar evolution for very massive stars

    第一類稱為恆星質量黑洞，這類黑洞的質量與太陽質量的量級相若，它們都是巨大恆星演化后的最終物。
  16. The black hole could then grow even stronger ( from the star ' s mass ) as to possibly absorb another

    吸收了恆星質量之後，黑洞進一步膨大，並有可能吞噬下一顆恆星。
  17. Many of these newly formed stars are very massive and race through their evolution to explode as supernovas

    許多新近形成的恆星質量都很大，並會快速演化到爆發的超新星。
  18. However, the massive star will have a shorter life span, for example, a 15 solar mass star can only survive for about 10 million years

    有趣的是，恆星質量越大，壽命越短，例如一顆相等於15個太陽質量的恆星，便只有一千萬年的壽命。
  19. After the process of matter ejection stellar body will continue collapsing into black hole if the mass of the nuclear - energy - exhausted star is more than 3 mq

    星體經過物質拋射后，核能耗盡的恆星質量超過3m _ ，則此星體將繼續坍縮成黑洞。
  20. Candidates for stellar - mass black holes were identified mainly by the presence of accretion disks of the right size and speed, without the irregular flare - ups that are expected from disks around other compact objects

    鑒別恆星質量黑洞主要靠合適大小和速度的增大圓盤的存在，沒有認為從其它緊密物體周圍閃耀的無規律的閃光。
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