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initial mass function中文是什么意思

  • 初始質(zhì)量函數(shù)
  • 起始質(zhì)量函數(shù)

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  • Comparing with the current observations , which include the number density distribution in space , mass function , etc . , the so - called standard modes for both the power law and gaussian cluster initial mass functions are selected among many runs of simulations . the deviation from the standard modes , which is resulted from the change of the parameter for the initial conditions , is discussed in detail . the discussion of the model parameters is also presented although they are adopted as the typical values based on previous work
    對(duì)應(yīng)一定的初始分布我們發(fā)現(xiàn)無(wú)論是冪律的還是對(duì)數(shù)高斯的球狀星團(tuán)初始質(zhì)量譜經(jīng)過(guò)長(zhǎng)時(shí)間的動(dòng)力學(xué)演化都會(huì)得到和現(xiàn)在銀河系觀(guān)測(cè)到的球狀星團(tuán)系統(tǒng)相符的對(duì)數(shù)高斯的質(zhì)量分布;動(dòng)力學(xué)演化會(huì)明顯地改變球狀星團(tuán)系統(tǒng)的空間密度分布,靠近銀心區(qū)域的球狀星團(tuán)瓦解得更多;經(jīng)過(guò)動(dòng)力學(xué)演化后的球狀星團(tuán)速度分布函數(shù)在靠近銀心的區(qū)域明顯得不同于初始分布,初始擁有較大軌道偏心率的球狀星團(tuán)更容易瓦解。
  • The number density distribution of globular cluster in space will change with time due to the dynamic evolution , especially for those in the central region of the galaxy ; 5 . for the power law initial cluster mass function , the peak value of the mass function after the dynamic evolution is sensitive to the lower limit of the initial mass function we adopt . the suggested value in this paper is - 104m , which is consistent with that reduced from the dynamical analyses for the giant molecular clouds
    對(duì)于冪率的初始質(zhì)量譜,球狀星團(tuán)系統(tǒng)動(dòng)力學(xué)演化后質(zhì)量分布的轉(zhuǎn)折點(diǎn)質(zhì)量主要是由初始質(zhì)量函數(shù)的質(zhì)量下限決定的,最為適合的值為10 ~ 4m _ ;冪率的初始質(zhì)量譜的譜指數(shù)對(duì)球狀星團(tuán)系統(tǒng)動(dòng)力學(xué)演化后質(zhì)量分布的轉(zhuǎn)折點(diǎn)質(zhì)量也有影響,其最佳值為1 . 5 2 . 0 ;經(jīng)過(guò)大約5gyr的動(dòng)力學(xué)演化,冪率的初始質(zhì)量譜就會(huì)演化成為高斯的對(duì)數(shù)質(zhì)量分布并具有在隨后的動(dòng)力學(xué)演化中保持對(duì)數(shù)高斯形式質(zhì)量分布的特性。
  • 百科解釋
The initial mass function (IMF) is an empirical function that describes the distribution of initial masses for a population of stars. The IMF is often given as a probability distribution function (PDF) for the mass at which a star enters the main sequence (begins hydrogen fusion).
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