neutron mass 中文意思是什麼
neutron mass
解釋
中子質量-
For example, if there is a planet orbiting around the neutron star, it will wobble a little and the pulses will come a little early or late. we can then deduce the mass and the radius of the orbit of the planet from the arrival time of the pulses. this is how the first extrasolar planet is discovered
例如假若有一顆行星圍繞一顆中子星運行，它會令中子星出現搖動，引致脈沖的間隔變長或短，由此我們根據脈沖周期的變化，可推斷出行星的質量和軌道半徑，這亦是天文學家找出第一顆地外行星時所用的方法。 -
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。 -
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。 -
Abstract : according to the observation of the number concentration spectrum and the mass concentration of atmospheric aerosol, tsp and its particle size distribution, micrometeorology, and the solar spectroscopic radiation, even the neutron activation treatment of sand dust samples in helan mountainous area, the formation law of sandstrom, dust and sand blowing weather and the characteristics of climatic variation in this area and the influence of helan mountain are counted and analysed
文摘:利用賀蘭山地區沙塵暴歷史資料和綜合觀測資料，對大氣背景、浮塵、揚沙和沙塵暴發生期間的大氣氣溶膠數濃度譜、質量譜、大氣總懸浮顆粒（ tsp ）及粒徑分佈、微氣象、分光日射觀測以及沙塵樣品進行中子活化處理，分析了該地區浮塵、揚沙和沙塵暴形成規律，氣候變化特徵和賀蘭山的影響。 -
According to the observation of the number concentration spectrum and the mass concentration of atmospheric aerosol, tsp and its particle size distribution, micrometeorology, and the solar spectroscopic radiation, even the neutron activation treatment of sand dust samples in helan mountainous area, the formation law of sandstrom, dust and sand blowing weather and the characteristics of climatic variation in this area and the influence of helan mountain are counted and analysed
利用賀蘭山地區沙塵暴歷史資料和綜合觀測資料，對大氣背景、浮塵、揚沙和沙塵暴發生期間的大氣氣溶膠數濃度譜、質量譜、大氣總懸浮顆粒（ tsp ）及粒徑分佈、微氣象、分光日射觀測以及沙塵樣品進行中子活化處理，分析了該地區浮塵、揚沙和沙塵暴形成規律，氣候變化特徵和賀蘭山的影響。 -
Since a 7 - solar - mass is too large to be a white dwarf or neutron star, it must be a black hole
因為有著7個太陽質量的星體不可能是白矮星或中於星，所以它一定是黑洞。 -
( 2000 ). the neutron irradiation is assumed to derive primarily by the reaction 13c ( a, n ) i60 with a minor contribution from the marginal burning of 22ne through the channel 22ne ( a n ) 23mg in the final, high temprature phase of each flash. and we considered the influence of the various parameters such as the initial core mass, the envelope mass, the mass - loss rate, the overlap factor and the delution factor etc., and we vary their value with the pulse number
本文採用分叉s -過程反應通道，以~ （ 13 ） c （ ， n ） ~ （ 16 ） o 、 ~ （ 22 ） ne （ ， n ） ~ （ 25 ） mg為雙脈沖中子源，用最新的中子俘獲截面，利用gallino和busso等人給出的agb星三殼層核合成模型，考慮到核心質量、挖掘程度、重疊因子、稀釋因子及星風質量損失率隨脈沖數的變化，詳細計算和研究了各個金屬豐度情況下的3m 。 -
To investigate the space / time distributions and occurrence and evolution of such events, the diffusion pattern over deserts, turbulent transfer features in sandstorm weather, the particle size distribution, mass concentration and its distribution, optic properties, chemical composition and physical factors responsible for the initiation of raising sands, we made integrative observation and sounding of sandstorms deep in the large - scale desert area, including tengri, badanjilin and maowusu, with the items consisting of micrometeorological measurement, 3d wind observation, data from kb - 120 and anderson samplers of mass concentrations of sands with their spectrum, the distribution of aerodynamic particle sizes from the aps3310a, retrieval of aerosols " optic depth from sunphotometer data, assay of the chemical composition by means of neutron activiation analysis ( naa ) and integrated study of all related factors for causing sandstorm to occur, based on the observations of all kinds
利用所取資料，系統分析了不同強度沙塵天氣條件下沙塵氣溶膠質量濃度和質量濃度譜、粒子譜分佈、光學厚度、化學組分等特徵；綜合分析了影響沙塵起動的諸物理因子在沙塵起動中的作用；用沙塵輸送模式對一次沙塵暴天氣造成的泥雨過程的形成機制進行了模擬。歷史氣象資料統計分析表明，沙塵暴有其高發期（ 4 、 5月）和高發時段（ 14 - 20時） ， 14時到20時之間發生的沙塵暴約占沙塵暴總次數的66 。揚沙和沙塵暴天氣條件下，湍流動量通量和湍流感熱通量都是重要的湍流交換，沙塵暴發生前近地層的超絕熱不穩定對沙塵暴天氣有加強作用。 -
A significant difference on the scalar self - energy and effective mass of neutrons in asymmetric nuclear matter, especially in neutron matter, is observed. the difference would result in an unreasonable sigh of the extracted effective couplings for isovector mesons
利用這樣的耦合常數在rmf近似下計算的核物質的結合能與dbhf結果會有偏離，因而得到的核狀態方程也會有偏離，如在飽和點處結合能有小於2的偏差。 -
In numeral simulation of passive neutron detection, it is proposed to use the iterative calculation in analyzing the neutron multiplication in nuclear warhead. on this basis, the mass of the plutonium pit could be obtained under some conditions
在被動中子探測數值模擬中，提出在確定了核彈頭的泄漏中子計數后，採用迭代方法計算中子在核彈頭模型中的增殖，由此在一定條件下可實施核彈頭質量屬性的反演。 -
That is the following in essence. a sufficient mass of cold matter will necessarily collapse to a black hole, and stars with different mass will evolve into the white - dwarf - star, the neutron - star or the black - hole eventually because of the radiation of the burning core. the collapse of stars with sufficient mass leads to a black hole endowed with mass and charge and angular momentum, no other adjustable parameters : " a black hole has no hair.
第二章簡單介紹一下「黑洞無毛」理論形成，即足夠質量的冷物質能夠塌縮成黑洞，不同質量的恆星由於核燃燒輻射最終會演化成為白矮星、中子星或黑洞，以及黑洞的終態系統唯一地由質量、電荷和角動量確定，而無其它物理參數，此即為「黑洞無毛」理論。 -
The isospin effect and k production in intermediate and high energy heavy ion collisions ( hics ) are hot topics in the nuclear physics. based on the isospin - dependent quantum molecular dyanmics ( iqmd ) model and self - consistent relativistic boltzmann - uehling - uhlenbeck ( rbuu ) model, we have studied them and obtained some interesting results. as for the study of isospin in intermediate energy hics, we ' ve investigated how both stength ( q ) and density dependence of symmetry potential ( sp ) affect many measurable observables, such as the yield, phase - space, and isospin distributions of fragments, as well as the correlations between intermediate - mass - fragment ( imf ) multiplicity n and charged - particle multiplicity n, light - charged - particle ( lcp ) multiplicity n, and neutron multiplicity n,
在中能重離子碰撞的同位旋研究方面，分別研究了對稱勢的強度（ c _ s ）和其密度依賴形式對中能重離子核反應各類碎片產物產額、相空間、及其同位旋的分佈，中等質量碎片多重數（ n _ （ imf ） ）與帶電粒子多重數（ n _ c ） 、輕帶電粒子多重數（ n _ k ） 、中子多重數（ n _ n ）的關聯等多種實驗觀測量的影響，以獲取對稱勢中該兩方面的信息，尤其著重於研究如何分別獲取有關該兩方面的信息的途徑。 -
The evolution of fixed star having something to do with nuclear reaction, the star generally loses partial mass in its final period and finally collapses into compact star ( white dwarf, neutron star or black hole )
恆星的演化與核反應有關，演化到晚期的恆星一般要損失一部分質量，然後坍縮成緻密星（白矮星、中子星或黑洞） 。 -
More recently, dr. rosanne di stefano also from the harvard - smithsonian centre for astrophysics and i used the chandra x - ray observatory to detect objects dubbed " quasisoft " x - ray sources in nearby galaxies because of their low temperatures, which are at most four million degrees celsius. that is well below the temperatures expected for " hard " x - ray sources such as neutron stars or stellar mass black holes - which run between 10 million and 100 million degrees celsius - and still hotter than " soft " x - ray sources like white dwarfs
最近羅珊迪史提芬路博士她亦來自哈佛大學史密森天體物理中心和筆者利用錢德拉射線天文臺在鄰近星系偵測到一種奇怪的-射線源，我們稱之為類軟射線源，因為它們的溫度最高只有攝氏400萬度，遠低於一般硬射線源，例如中子星和恆星型黑洞溫度介乎攝氏1千萬至1億度，卻又比軟射線源例如白矮星為高。 -
The temperature range of quasisoft x - ray sources falls just right for an accreting black hole that is more massive than a stellar - mass black hole. however, we should be cautioned that in principle, the low temperatures of many quasisoft x - ray sources can be explained by stellar - mass black holes, neutron stars, and even white dwarfs under very specific physical conditions
就以類軟射線源的溫度范圍來說，雖然它完全符合那些比恆星型黑洞更大的吸積黑洞，但有一點不能忽略，就是這個溫度在理論上也可以是由恆星型黑洞中子星甚至白矮星在一些特殊物理情況下產生。 -
We take 3. 5 solar masses as the benchmark for judging whether something is a black hole because we know we know that theoretically the mass of other compact objects like neutron star cannot exceed that maximum threshold. otherwise those bodies will collapse under their own gravitational force into black holes
我們以質量大於太陽的3 . 5倍作為判別黑洞的標準，是因為從理論上得知，其他緻密天體如中子星的質量都不可能超越這個上限，否則它們便會因為本身的重力而塌縮成黑洞。 -
In this model, neutron star ' s maximum mass is 1. 12ms, with corresponding radius about 8km
在我們的模型中，中子星最大質量極限為1 . 12ms （ ms為太陽質量） ，對應半徑約為8km 。 -
Such a process can take place in the low mass x - ray binary systems where the mass transfer from the companion to the neutron star can be larger than 0. 5 solar masses. if the neutron star in the low mass x - ray binary accretes the matter, the central densities can reach to a state that strange - matter seeds are formed in the interiors of the star
在這個系統內，中子星可能會吞噬超過0 . 5個太陽質量的伴星物質，當中子星吸收了這些物質后，中心的密度會增加至足以產生奇異物質種子，這些種子會開始吞噬四周的中子物質，釋放出大量中微子和反中微子，令星體冷卻。 -
Higher mass stars will die in spectacular stellar explosions called supernovae, leaving behind even more compact objects - neutron stars for stars of mass lower than 25 solar masses and black holes for stars of mass higher than 25 solar masses
一些質量大於8個太陽質量但少於25個太陽質量的恆星在超新星爆發后會成為中子星，而質量大於25個太陽質量的恆星最終會演化成黑洞。 -
Their detailed origin remains unknown. that doesn t stop the astronomers from guessing though ! amongst the candidates are the collapse of supermassive stars over 60 times the mass of the sun, mergers of two neutron stars, or conversion of a neutron star to a strange star
另一方面，伽瑪射線爆發是發生在宇宙深處一種最強烈的爆炸，雖然至今而人們還未弄清它們的來源，但是這並沒有令天文學家放棄推測，其中的一些猜想，包括比太陽質量大60倍的巨型恆星正在塌縮兩顆中子星合併，或是中子星變為奇異星。
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