星系暈 的英文怎麼說
中文拼音 [xīngxìyūn]
星系暈
英文
galactic halo-
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。Our results are much helpful for us to understand the building - up mechanism of the universal density profile, galaxy formation and high redshift tully - fisher relation
這些結果對我們解釋暗暈的普適密度輪廓，高紅移盤星系的瓜111卜f討ler關系和理解星系核球及盤的形成都有很大幫助At least some elliptical galaxies, as well as the bulges and halos of spiral galaxies, may have arisen from such collisions
至少螺旋星系的核球與暈，以及某些橢圓星系，可能是由此種碰撞產生的。We find that within a given cosmological model different schemes of galaxy formation lead to significant changes of the pvd. we propose a simple phenomological model for the formation of lyman break galaxies, determined by the formation interval parameter z and the halo mass threshold mh
首先，我們提出了一個簡單唯象模型來聯系宇宙學n體數值模擬和lymanbreak星系，該模型由兩個參量（形成時間間隔_ z和暗暈質量下限m _ h ）唯一確定。With a reasonable choice for these two parameters, our model predicts an occupation number distribution of galaxies in halos which agrees very well with the predictions of semi - analytical models
通過適當選擇這兩個參量，模型預言的暗暈中星系的分佈函數和半解析模型的結果符合得非常好。For the galaxy, a model contained three components ( bulge, disk and halo ) suggested by paczynski ( 1990 ) is adopted, which can reproduce most of the global observational properties of the milky way such as the rotation curve
動力學演化的時間取為銀河系球狀星團的平均年齡12gyr 。我們採用了三成分（核球、盤、暈）的銀河系模型（ p90 ） 。Another intriguing feature of quasisoft x - ray sources is that they locate at different type of galaxies like spirals and ellipticals. quasisoft x - ray sources are also found in the halos of galaxies and even in globular clusters
類軟天體另一有趣之處，是它們不單盤踞在旋渦或橢圓等不同類型星系內，在銀暈甚至球狀星團中竟亦見其蹤影。The visible parts of galaxies are believed to be enveloped in giant “ halos ” of dark matter
我們相信，星系中可以看得見的部分，其實是籠罩在巨大的黑暗物質暈里。On larger scales, analogous halos are thought to keep clusters of galaxies bound together
在更大的尺度上，有人相信，由於存在著類似的暈體，星系團才凝聚在一起。分享友人