本文關(guān)鍵詞：球狀星團(tuán)M2中恒星元素的天體物理來源探究　出處：《河北師范大學(xué)》2017年碩士論文　論文類型：學(xué)位論文

  更多相關(guān)文章： 球狀星團(tuán) 元素 豐度 貢獻(xiàn)

【摘要】：我們的宇宙大約形成于140Gyr年前的一次大爆炸。球狀星團(tuán)是星系中古老的、壽命很長(zhǎng)的成員,被稱為星系演化的活化石。觀測(cè)表明,球狀星團(tuán)M2中α元素、Fe族元素和中子俘獲元素的豐度隨樣本星[Fe/H]的變化呈現(xiàn)出不同的變化趨勢(shì)。對(duì)樣本星中元素豐度來源的研究可以幫助我們更好的理解球狀星團(tuán)M2形成的歷史和化學(xué)演化進(jìn)程。本文主要包括兩部分:第一部分首先給出了獨(dú)立于星系化學(xué)演化的五分量元素豐度模型及其計(jì)算方法。其次對(duì)球狀星團(tuán)M2中14顆樣本星(6顆r-only星,4顆s星,4顆metal rich星)的元素豐度進(jìn)行了擬合,并給出了最佳擬合結(jié)果。通過對(duì)計(jì)算結(jié)果的系數(shù)分布情況進(jìn)行分析得出,在樣本星所觀測(cè)的金屬豐度范圍內(nèi),r-過程分量對(duì)元素豐度的貢獻(xiàn)一直處于主要地位。weak s-過程分量和SNe Ia分量雖然對(duì)元素豐度的貢獻(xiàn)較少,但是隨著[Fe/H]的增大其貢獻(xiàn)也緩慢增加。4顆s星具有典型的s-過程特征,s-過程貢獻(xiàn)超豐。另外,文中給出的整體擬合效果圖也驗(yàn)證了我們的計(jì)算方法是可行有效的。第二部分對(duì)計(jì)算結(jié)果給出了分析和討論。對(duì)樣本星的α元素、Fe族元素和中子俘獲元素的天體物理來源進(jìn)行了分析討論,并給出了本文的結(jié)論。本文所選取樣本星的觀測(cè)金屬豐度范圍較窄(-1.8[Fe/H]-0.9),在觀測(cè)范圍內(nèi),大質(zhì)量星的primary過程分量對(duì)α元素和Fe族元素豐度的貢獻(xiàn)都起了明顯的主導(dǎo)作用,并且primary分量對(duì)α元素和Fe族元素的貢獻(xiàn)隨著[Fe/H]的增加,呈現(xiàn)出不同程度的緩慢下降的趨勢(shì)。與此同時(shí),SNe Ia分量和大質(zhì)量星的secondary過程分量對(duì)α元素和Fe族元素豐度的貢獻(xiàn)隨著樣本星[Fe/H]的增加緩慢上升。較輕的中子俘獲元素Y元素和Zr元素的豐度主要是來源于main s-過程分量和week r-過程分量,其對(duì)元素豐度的貢獻(xiàn)隨[Fe/H]的增加變化緩慢;而較重的中子俘獲元素的天體物理來源為main r-過程分量和main s-過程分量,對(duì)于比Eu重的元素,main r-過程分量的貢獻(xiàn)作用一直處于主導(dǎo)地位。4顆s星在樣本星中比較特別,main s-過程分量對(duì)其元素豐度的貢獻(xiàn)超豐,這可能與其受到了低質(zhì)量AGB星的污染有關(guān)。
[Abstract]:Our universe was formed about a big bang 140Gyr years ago. Globular cluster is an old and long life member of the galaxy, known as a living fossil of the evolution of galaxies. The observations show that the abundance of alpha, Fe and neutron capture elements in the globular cluster M2 varies with the variation of the sample star [Fe/H]. The study of the source of the element abundance in the sample star can help us better understand the history and chemical evolution process of the formation of the globular cluster M2. This paper mainly consists of two parts. In the first part, the five component element abundance model independent of the evolution of Galaxy chemistry and its calculation method are given. Secondly, the element abundance of 14 sample stars (6 r-only stars, 4 s stars, 4 metal rich stars) in the globular cluster M2 is fitted, and the best fitting results are given. Through the analysis of the coefficient distribution of the calculated results, it is concluded that the contribution of the r- process components to the abundances of elements is always in the leading position in the range of metallicity observed by the sample stars. The contribution of the weak s- process component and the SNe Ia component to the element abundance is less, but with the increase of [Fe/H], its contribution also increases slowly. The 4 s stars have typical s- process features, and the s- process has a great contribution. In addition, the overall fitting effect diagram presented in this paper also proves that our calculation method is feasible and effective. The second part gives the analysis and discussion of the calculation results. The astrophysical sources of the alpha, Fe and neutron capture elements of the sample star are analyzed and discussed, and the conclusion of this paper is given. This paper observed metallicity range sample stars narrow (-1.8[Fe/H]-0.9), in the observation range, the contribution of primary component star of alpha elements and Fe group element abundances have played a leading role obviously, and the primary component of alpha elements and Fe elements contribution with the increase of [Fe/H], showing different degrees of slow decline. At the same time, the contribution of the secondary process component of the SNe Ia component and the mass star to the abundances of the alpha and Fe elements increases slowly with the increase of the sample star [Fe/H]. The abundance of lighter neutron capture elements Y and Zr elements are mainly derived from the main s- component and week r- component, the contribution of element abundance changes slowly with the increase of [Fe/H]; and astrophysical sources of heavier neutron capture elements for the main r- component and main s- component, for more than Eu heavy elements, the contribution main r- process component has been in a dominant position. The 4 s stars are more special among the sample stars, and the component of the main s- process contributes to the abundance of its element abundance, which may be related to the pollution of low mass AGB stars.
【學(xué)位授予單位】：河北師范大學(xué)
【學(xué)位級(jí)別】：碩士
【學(xué)位授予年份】：2017
【分類號(hào)】：P154.12

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