metallicity 中文意思是什麼

metallicity 解釋
金量
  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. High - metallicity cluster

    高金屬度星團
  3. The high metallicity of disk gcs was caused by the particular environment they are situated. because of the strong interaction wjth the disk, the extent of outflow and star formation efficiency ( sfe ) of the disk gcs was quite different from the halo gcs, which leads to the significant difference between the metallicity distribution of two classes of gcs

    本文建立的自增豐演化模型對球狀星團的余屬度雙峰分佈提出了一種新的解釋，指出盤族球狀星團之所以出現較高的金屬度，是因為它處于銀盤這一特殊的環境下，與銀盤相互作用而造成比暈族球狀星團更為強烈的增豐。
  4. The differences in orbital morphologies due to different potentials is slighting, however, given a certain potential, for clusters that have perigalactic distance smaller than 1 kpc, some orbits may exhibit a chaotic behavior. the correlation between the metallicity of samples and the orbital morphologies is unclearly ; ( 4 ) it is found that the semi - major axis, apogalactic distance and azimuth period of 29 sample clusters are changed with their metallicity similarly, but a obvious correlation is seen between orbital eccentricity and metallicity. there is a fraction of 24 % of the sample clusters with eccentricities lower than 0. 4

    不同的引力勢模型對球狀星團軌道的具體形態影響不大，在給定的引力勢模型下，當某些星團的運動軌道穿越距銀心1kpc附近的區域時會出現「混沌」現象： （ 4 ） 29個樣本星團的軌道半長軸、遠銀心距和方位周期隨金屬度的變化規律基本相似，樣本星團的金屬度與其軌道形態之間的相關性並不明顯，然而軌道偏心率與金屬度有關，對于所選的暈族樣本星團而言，大約有24的樣本星團的軌道偏心率低於0 . 4 。
  5. Our yields increase with the mass of the progenitor main - sequence stars. massive stars ( i. e. 18m < m < 50m ) is the primary sites of the neclearsynthesis of the r - process and can explain the galaxy chemical evolution. 3. we present formula to calculat the r - process galactic chemical evolution of ba peak elements. this formula contains metallicity abundance and point out the relation of the ba peak elements and disscuss the effect of various mass supersnova. besides, our formula can be confirmed by a lot of observations

    由此可以解釋以下觀測事實: （ l ） mg ， eu均產生於snh星，但質量范圍不同，在高質量（ > 20 ） eu的產量高， mg的產量（相對于太陽） ，導致暈星中eu / mg > 0 ，而產生mg的質量范圍較大，致使在厚盤的晚期較小質量超新星也開始對mg有貢獻，而這些星對eu的貢獻很小，致使在厚盤星中eu / mg < 0 ，在厚盤中eu / fe隨金屬豐度的升高而降低，仁mg / fe隨金屬豐度的升高而不變
  6. The calculating results show : ( 1 ) most of samples are located in 5 kpc - 10 kpc from galactic center. all of the sample clusters present a spherical symmetrical distribution around the galactic center, and their space velocities are presented a ellipsoidal distribution ; ( 2 ) according to the metallicity and basic characters, the sample clusters are separated into hb subgroup and mp subgroup. the number of samples are changed with metallicity [ fe / h ], and there is a peak at [ fe / h ] = - 1. 6 ; ( 3 ) the orbits of sample clusters show mostly limited, periodic characteristics, but the orbits are not closed completely, their maximal galactocentric distance is less than 40 kpc

    計算結果表明： （ 1 ）大部分樣本星團都位於銀心距5kpc 10kpc的范圍內，相對于銀心呈球對稱分佈，它們的速度也呈橢球分佈； （ 2 ） 29個樣本星團按其金屬度大小和基本性質分類，可分屬hb和mp兩個球狀星團次系，且樣本星團數隨金屬度[ fe h ]而變化，在[ fe h ] = - 1 . 6處出現一個峰值； （ 3 ）所有樣本星團的軌道運動都呈周期性，大都在一個有界而不封閉的周期軌道上運動，其最大銀心距都在40kpc以內。
  7. Our model introduces the general equations of chemical evolution used in galaxies to studies of gcs. in this model the important gas outflow caused by the supernova explosion and other processes during the formation of globular clusters is included. based on such a self - enrichment model, monte carlo method is used to simulate the formation and chemical evolution of globular cluster systems, from which a new explanation of the bimodal metallicity distribution can be given

    本文把星系演化中通用的化學演化方程引入到球狀星團這一系統中來，特別考慮到球狀星團中恆星形成過程中超新星爆發等因素引發的氣體外流，把這一重要的物理過程包含到化學演化方程中，並用蒙特卡羅方法來模擬球狀星團系統的自增豐演化。
  8. 2. the abundance distributions of the sbl component part with 92 a132 are nearly similar to the solar pattern at any metallicity

    S _ （ ml ）分佈與太陽系有差異，但對于質量范圍92 a 132 ，任何金屬豐度下分佈與太陽系相應分量大體相似。
  9. Thus the cumulative consequence of galactic chemical evolution starting from low metallicity agb stars, namely, the average abundance patterns of sbh part with 140a204 ( or the snl component part with 92a132 ) in different metal conditions, should be similar ( ornearly similar ) to the corresponding solar s - bajn component

    低金屬豐度條件下，由於中子輻照量隨金屬豐度的降低而升高， s _ （ ml ）產量低於s _ （ mh ） 。雖然s _ （ ml ）分佈與太陽系有差異，但對于質量范圍92 a 132 ，任何金屬豐度下分佈與太陽系大體相似。
  10. Low - metallicity cluster

    低金屬度星團
  11. It is also pointed out that the " pre - enrichment " ca n ' t be used to explain the bimodal structure of metallicity distribution of gcs

    本文的研究同時指出， 「預增豐」不可能造成球狀星團系統的金屬度雙峰結構。
  12. Consequently the distributions of the corresponding solar s, h component is typical and can serve as a standard pattern in investigating the abundance distribution of neutron capture elements at any metallicity

    因而太陽系的s _ （ ml ）的88 a 138部分可以近似做為任何金屬豐度情況下的標準豐度分佈模式。一s
  13. It has long been known from observations that the metallicity distribution of galactic gcs shows bimodal structure. in recent years the same distribution feature has also been found in other galaxies. how to explain this phenomenon is a challenge to the formation and evolution of gcs

    觀測發現銀河系和其它星系中的球狀星團系統普遍表現出類似的金屬度分佈雙峰結構，這一分佈特徵成為研究球狀星團形成與演化極為重要的觀測約束條件。
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