質量過大恆星 的英文怎麼說

中文拼音 [zhíliángguòdàhéngxīng]
質量過大恆星 英文
overmassive star
  • 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
  • 過 : 過Ⅰ動詞[口語] （超越） go beyond the limit; undue; excessiveⅡ名詞（姓氏） a surname
  • 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...
  • 恆星 : [天文學] fixed star; star恆星大氣 stellar atmosphere; 恆星導航 star navigation; stellar guidance;...
  1. 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。
  2. To search for high - velocity molecular emission toward massive star formation regions, and to study the connections between h2o masers, iras objects and outflow properties, we carried out a co observation for a h2o maser sample. we found that most of the objects have excess high velocity emission produced by outflows ; we find a significant correlation between co line full widths and iras luminosities. the widths are proportional to the iras luminosities

    通過在大質量恆星形成區搜尋高速分子輻射，並且研究它們與星際h _ 2o脈澤源和所聯系的紅外源之間的關系，我們發現絕大多數源都存在著氣體的高速運動並且它們是由分子外流產生的；我們同時發現在co分子的譜線全寬和所對應源的紅外光度之間存在很好的相關性，線寬隨紅外光度增加而變大。
  3. 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。
  4. They are the stellar evaporation in the tidal field, the stellar evolution during the early evolutionary stage, the tidal shocks due to clusters passing through the bulge and disk, and the dynamical friction

    本文考慮的動力學過程有四種，即：恆星蒸發、早期大質量恆星的演化、銀河系核球和盤的沖擊加熱以及動力學磨擦。
  5. The helium will burn steadily and the higher energy production rate will heat up the star. the star will swell to a size even larger than a red giant and we have a

    在恆星強大質量的約束下，核心氦聚變成碳的過程能穩定地進行，在核心高熱的煎熬下，恆星外殼會極度膨脹成為比紅巨星更巨大的
  6. After 100, 000 to one million years, depending on the original mass of the star, it ceases altogether, and the remnant star settles down as an extremely dense and hot white dwarf ? a stellar ember crushed by gravity into a nearly crystalline orb about the size of earth

    經過10 ~ 100萬年（取決于恆星的原始質量） ，恆星風將驟然終止，而恆星的殘留物會演變成極緻密高熱的白矮星：一種被重力擠壓成地球般大小，近乎晶質球體的恆星遺骸。
  7. There are two different ideas about the massive star formation. some investigators suggest that high - mass stars form via dynamical collapse of cloud cores, resulting in disk accretion and molecular outflows, similar to their low - mass counterparts ; some peoples suggest that high - mass stars form by the coalescence of low - to intermediate - mass stars

    關于大質量恆星的形成有兩種觀點：一種觀點認為大質量恆星通過雲核的塌縮，然後產生一個吸積盤和外流，即相似於低質量恆星的形成；另一種觀點認為大質量恆星通過中小質量的恆星併合而成。
  8. At the other extreme, a star whose mass is too great will become so hot as a result of accelerated nuclear reaction.

    另一極端方面，質量過大的恆星將會由於加快了原子核反應而變得很熱。
  9. Supermassive black holes containing millions to billions of solar masses could also form wherever a large number of stars are packed in a relatively small region of space, or by large amounts of mass falling into a " seed " black hole, or by repeated fusion of smaller black holes

    超大質量的黑洞包含數百萬到幾十億的太陽質量，無論大量恆星聚集在一相對地小的空間區域里也可以形成黑洞，或通過大量質量落下進入一個「種子」黑洞之內，或通過反復融合比較小的黑洞。
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