metallicity造句
例句与造句
- High - metallicity cluster
高金属度星团 - Low - metallicity cluster
低金属度星团 - It is also pointed out that the " pre - enrichment " ca n ' t be used to explain the bimodal structure of metallicity distribution of gcs
本文的研究同时指出， “预增丰”不可能造成球状星团系统的金属度双峰结构。 - 2 . the abundance distributions of the sbl component part with 92 a132 are nearly similar to the solar pattern at any metallicity
S _ ( ml )分布与太阳系有差异，但对于质量范围92 a 132 ，任何金属丰度下分布与太阳系相应分量大体相似。 - 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
因而太阳系的s _ ( ml )的88 a 138部分可以近似做为任何金属丰度情况下的标准丰度分布模式。一s - It's difficult to find metallicity in a sentence. 用metallicity造句挺难的
- 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
观测发现银河系和其它星系中的球状星团系统普遍表现出类似的金属度分布双峰结构，这一分布特征成为研究球状星团形成与演化极为重要的观测约束条件。 - 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
不同的引力势模型对球状星团轨道的具体形态影响不大，在给定的引力势模型下，当某些星团的运动轨道穿越距银心1kpc附近的区域时会出现“混沌”现象： ( 4 ) 29个样本星团的轨道半长轴、远银心距和方位周期随金属度的变化规律基本相似，样本星团的金属度与其轨道形态之间的相关性并不明显，然而轨道偏心率与金属度有关，对于所选的晕族样本星团而言，大约有24的样本星团的轨道偏心率低于0 . 4 。 - 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学演化方程引入到球状星团这一系统中来，特别考虑到球状星团中恒星形成过程中超新星爆发等因素引发的气体外流，把这一重要的物理过程包含到化学演化方程中，并用蒙特卡罗方法来模拟球状星团系统的自增丰演化。 - 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
本文正是在银河系化学演化的基础上，利用银河系的三成分( threezone ) (即晕、厚盘和薄盘)多相( multi - phase ) (气体，分子云，大、小质量恒星以及剩余物质)的化学演化的理论模型，通过与观测约束(质量面密度、场星的年龄-金属丰度关系、太阳附近g矮星金属含量分布函数、三成份的特征量、元素的星系化学演化、超新星的爆炸率、内落速率等)的比较，来检验模型的合理性。 - 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
计算结果表明： ( 1 )大部分样本星团都位于银心距5kpc 10kpc的范围内，相对于银心呈球对称分布，它们的速度也呈椭球分布； ( 2 ) 29个样本星团按其金属度大小和基本性质分类，可分属hb和mp两个球状星团次系，且样本星团数随金属度[ fe h ]而变化，在[ fe h ] = - 1 . 6处出现一个峰值； ( 3 )所有样本星团的轨道运动都呈周期性，大都在一个有界而不封闭的周期轨道上运动，其最大银心距都在40kpc以内。 - 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
低金属丰度条件下，由于中子辐照量随金属丰度的降低而升高， s _ ( ml )产量低于s _ ( mh ) 。虽然s _ ( ml )分布与太阳系有差异，但对于质量范围92 a 132 ，任何金属丰度下分布与太阳系大体相似。 - 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
本文建立的自增丰演化模型对球状星团的余属度双峰分布提出了一种新的解释，指出盘族球状星团之所以出现较高的金属度，是因为它处于银盘这一特殊的环境下，与银盘相互作用而造成比晕族球状星团更为强烈的增丰。 - 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
由此可以解释以下观测事实: ( l ) mg ， eu均产生于snh星，但质量范围不同，在高质量( > 20 ) eu的产量高， mg的产量(相对于太阳) ，导致晕星中eu / mg > 0 ，而产生mg的质量范围较大，致使在厚盘的晚期较小质量超新星也开始对mg有贡献，而这些星对eu的贡献很小，致使在厚盘星中eu / mg < 0 ，在厚盘中eu / fe随金属丰度的升高而降低，仁mg / fe随金属丰度的升高而不变
