本文選題：銀河系 + 恒星�。� 參考：《河北師范大學(xué)》2011年碩士論文

【摘要】：太陽附近長(zhǎng)壽命的F和G型矮星被稱為銀河系演化的活化石,其恒星大氣的元素豐度直接反映了銀河系不同演化階段的化學(xué)成分,為研究銀河系的結(jié)構(gòu)和化學(xué)演化提供了強(qiáng)有力的探針。因此,這類恒星一直是天文學(xué)的主要觀測(cè)目標(biāo)。 我們的工作主要是大樣本恒星豐度的統(tǒng)計(jì)分析,我們的統(tǒng)計(jì)數(shù)據(jù)包括兩部分:第一部分是我們使用國(guó)家天文臺(tái)興隆觀測(cè)站2.16米望遠(yuǎn)鏡及其附屬的折軸攝譜儀,得到的102顆F和G型矮星的高分辨率、高信噪比光譜,利用MIDAS軟件包進(jìn)行光譜數(shù)據(jù)處理得到譜線的等值寬度,利用恒星大氣模型和原子譜線參數(shù),得到了O、Mg、Si、Ca、Ti等α元素的化學(xué)豐度。第二部分是大樣本的恒星元素統(tǒng)計(jì),選取了17篇文獻(xiàn)。兩部分樣本共得到了1161顆F和G型矮星(去除重復(fù)的恒星),根據(jù)純運(yùn)動(dòng)學(xué)判據(jù)確定了每顆恒星的星族成分,其中薄盤星為672顆,厚盤星為281顆,暈星為60顆,其余48個(gè) 樣本星為過渡恒星。我們的目的是通過大樣本的統(tǒng)計(jì)工作,分析α元素(Mg、Si、Ca、Ti)豐度和O元素豐度在不同星族成分中的分布趨勢(shì),進(jìn)而研究不同星族恒星的化學(xué)演化,為銀河系的形成和化學(xué)演化模型提供可靠的觀測(cè)約束。論文的第一部分首先簡(jiǎn)單介紹了樣本的選取標(biāo)準(zhǔn)和選取結(jié)果,并詳細(xì)分析了的樣本的完備性,討論了不同樣本之間豐度彌散。第二部分介紹了恒星運(yùn)動(dòng)學(xué)的有關(guān)知識(shí)和星族的劃分方法,計(jì)算了樣本恒星的空間速度并確定了樣本的星族成分。第三部分詳細(xì)討論了不同星族恒星α元素豐度[α/Fe]的演化趨勢(shì),并討論分析了銀盤恒星α元素的豐度梯度。最后一部分是結(jié)論和討論。 通過對(duì)太陽附近1113顆矮星的高分辨率光譜分析得到的元素豐度的統(tǒng)計(jì)分析,獲得到如下一些重要結(jié)果: (1)金屬豐度分布:薄盤恒星的金屬豐度范圍為-1.0[Fe/H]+0.5;厚盤恒星的金屬豐度范圍為-3.0[Fe/H]+0.5,覆蓋整個(gè)樣本的金屬豐度范圍;暈族恒星的金屬豐度范圍為-3.0[Fe/H]-0.7。因此,厚盤與薄盤恒星、厚盤與暈族恒星以及薄盤與暈族恒星的金屬豐度都存在交叉重疊區(qū)域,不能從金屬豐度上嚴(yán)格區(qū)分三個(gè)不同的星族成分。 (2)平均銀心距分布:薄盤恒星的R~m= 5.5~10.0 kpc,主要分布在7.0 ~9.0kpc范圍內(nèi);厚盤恒星的R~m= 4.0 ~ 11.0 kpc,主要分布在5.5 ~7.5kpc范圍內(nèi);暈族恒星的R~m= 4.0 ~ 10.0 kpc,主要分布在4.5 ~6.0kpc范圍內(nèi)�？梢�,薄盤、厚盤和暈族恒星的平均軌道半徑分布也是相互重疊的,不能嚴(yán)格區(qū)分。 (3)最大法向距分布:薄盤恒星在垂直銀道面方向的最大法向距Z_(max)1kpc;厚盤恒星的Z_(max)=0.1 ~ 4kpc;暈族恒星的Z_(max)1kpc。因此,薄盤與厚盤之間、厚盤與暈族恒星之間的最大法向距也存在部分重疊,不能嚴(yán)格區(qū)分。 (4)α元素(Mg、Si、Ca、Ti)的豐度[α/Fe]在貧金屬星中相對(duì)超豐,但4種α元素的演化趨勢(shì)并不完全一致,而且[α/Fe]隨金屬豐度[Fe/H]的演化趨勢(shì)在薄盤和厚盤恒星中也是不同的。薄盤恒星中4種α元素的豐度[α/Fe]隨[Fe/H]的增加呈線性下降趨勢(shì),到達(dá)太陽金屬豐度[Fe/H]=0時(shí)達(dá)到太陽系的豐度即[α/Fe]=0。厚盤恒星中[α/Fe]隨[Fe/H]的增加并非呈單調(diào)下降趨勢(shì),而且[Mg/Fe]的演化趨勢(shì)與其它3種α元素Si、Ca、Ti的演化也不完全一致:其中[Mg/Fe]在[Fe/H]-1.5時(shí)隨[Fe/H]的增加呈線性下降趨勢(shì),在[Fe/H] = -2.0～-0.7之間[Mg/Fe]幾乎呈平臺(tái)分布,但當(dāng)[Fe/H]-0.7時(shí)[Mg/Fe]又隨[Fe/H]的增加迅速下降直到太陽系的豐度值;而其它3種α元素Si、Ca、Ti的豐度[X/Fe]一直隨[Fe/H]的增加呈線性下降趨勢(shì),但在整個(gè)金屬豐度范圍內(nèi)并不是單一斜率下降,而是在[Fe/H] = -0.7處存在一個(gè)突然下降的“膝點(diǎn)”,即[α/Fe]隨金屬豐度[Fe/H]增加到達(dá)[Fe/H] = -0.7附近時(shí)有個(gè)突然的加速下降。 (5)在厚盤和薄盤恒星金屬豐度相互重疊區(qū)域-1.0[Fe/H]+0.5內(nèi),厚盤恒星與薄盤恒星之間的[α/Fe]是混合在一起的,不能依據(jù)α元素豐度如[Mg/Fe]的大小嚴(yán)格地區(qū)分厚盤和薄盤恒星,但厚盤恒星[α/Fe]豐度的平均值明顯高于薄盤恒星。 (6)對(duì)富金屬的薄盤恒星([Fe/H]0)來說,4種α元素Mg、Si、Ca、Ti的相對(duì)豐度[α/Fe]隨金屬豐度[Fe/H]的演化趨勢(shì)各不相同:[Mg/Fe]隨[Fe/H]的增加繼續(xù)下降到低于太陽系的豐度;[Si/Fe]和[Ca/Fe]在[Fe/H]0時(shí)保持太陽系豐度值不變;[Ti/Fe]隨著[Fe/H]的升高有微弱的增加趨勢(shì)。 (7)[O/Fe]隨[Fe/H]的演化趨勢(shì)與[Mg/Fe]一致,但薄盤恒星[O/Fe]在[Fe/H]≈-0.4處存在一個(gè)膝狀下降。而[α/O]隨[O/H]的增加而線性下降,薄盤和厚盤的[α/O]也存在混合,不能嚴(yán)格區(qū)分,且厚盤星的豐度彌散較薄盤星大。 (8)無論是厚盤、薄盤還是暈族恒星的[α/Fe]豐度都與恒星形成時(shí)的平均軌道半徑R~m、以及離開銀道面的最大距離Z_(max)分布無關(guān),即不存在α元素豐度梯度。薄盤和厚盤的α元素豐度[α/Fe]在R~m=7kpc時(shí)是勉強(qiáng)能夠分開的,但是還是有一部分的厚盤星與薄盤星混合;在銀盤縱向上,在Z_(max)=1kpc時(shí)薄盤和厚盤的α元素豐度[α/Fe]可以分開,但是同樣有部分厚盤星混合在薄盤區(qū)域內(nèi)。在Z_(max)=4kpc時(shí),厚盤和暈星的[α/Fe]能夠明顯分開。 (9)薄盤、厚盤和暈族恒星的運(yùn)動(dòng)學(xué)性質(zhì)明顯不同,其中繞銀心旋轉(zhuǎn)的軌道速度VLSR的區(qū)分更加明顯,薄盤恒星:V_(LSR)-60km/s,且V_(total)90km/m;厚盤恒星:-180km/sV_(LSR)-60km/s,且250V_(total) 90km/m;暈族恒星:V_(LSR)-180km/s,且V_(total) 200 km/s。此外,三個(gè)星族成分的速度彌散也不同,由薄盤到厚盤再到暈星的速度彌散依次增大。但恒星的α元素豐度[α/Fe]與運(yùn)動(dòng)學(xué)速度之間沒有相關(guān)性,且既存在一些具有典型薄盤恒星[α/Fe]豐度而運(yùn)動(dòng)學(xué)上屬于厚盤的恒星,也存在一些具有典型厚盤恒星[α/Fe]豐度而運(yùn)動(dòng)學(xué)上屬于薄盤的恒星。 (10)暈族恒星的[α/Fe]豐度也呈現(xiàn)隨[Fe/H]增加而下降的趨勢(shì),但暈族恒星[α/Fe]豐度的彌散遠(yuǎn)大于豐度的分析誤差,且與厚盤恒星的α元素豐度存在嚴(yán)重的混合,存在一些[α/Fe]豐度低于薄盤的所謂貧α元素暈星。這些統(tǒng)計(jì)結(jié)果表明,雖然平均來講厚盤恒星的[α/Fe]豐度高于薄盤恒星,但在金屬豐度重合區(qū)域內(nèi)[α/Fe]也是相互交叉混合的,不能嚴(yán)格區(qū)分。這與近年來單個(gè)樣本的觀測(cè)結(jié)果不同。因此,關(guān)于薄盤和厚盤恒星的α元素豐度是否區(qū)分,還需要更多的大樣本觀測(cè)數(shù)據(jù)來的確認(rèn)。
[Abstract]:The long-lived F and G dwarf stars in the vicinity of the sun are known as the living fossil of the Milky way evolution. The element abundance of the star atmosphere directly reflects the chemical composition of the different evolution stages of the Milky way, providing a powerful probe for the study of the structure and chemical evolution of the Milky way.
Our work is mainly the statistical analysis of the abundance of large sample stars. Our statistics include two parts. The first part is the high resolution, high signal to noise ratio spectrum of 102 F and G dwarf stars, and the spectrum of the high signal to noise ratio, using the MIDAS software package. The chemical abundances of O, Mg, Si, Ca, Ti and other alpha elements are obtained by using the stellar atmosphere model and the parameters of the atomic spectral line. The second part is the stellar element statistics of large samples, and 17 articles are selected. The two parts of the samples have obtained 1161 F and G Dwarfs (removal of repeated stars), according to the pure kinematic criteria. The star composition of each star is determined, of which 672 are thin disk stars, 281 thick disk stars, 60 halo stars, and the remaining 48.
The sample star is a transition star. Our aim is to analyze the distribution trend of the abundance of alpha elements (Mg, Si, Ca, Ti) and the abundance of O elements in different star composition by large sample statistics, and then study the chemical evolution of different star stars and provide reliable observation constraints for the formation and chemical evolution model of the galaxy. Firstly, the criteria and results of sample selection are briefly introduced, and the completeness of the samples is analyzed in detail. The abundance dispersion between different samples is discussed. The second part introduces the related knowledge of the stellar kinematics and the division method of the star family, calculates the space velocity of the sample star and determines the Star composition of the sample. The third part of the sample is determined. The evolution trend of alpha element abundances (alpha /Fe]) in different star stellar stars is discussed in detail, and the abundance gradient of alpha elements in a silver disk star is discussed and analyzed. The last part is the conclusion and discussion.
Based on the statistical analysis of elemental abundance obtained by high-resolution spectral analysis of 1113 dwarfs near the sun, the following important results are obtained:
(1) distribution of metallicity: the metallicity of a thin disk star is -1.0[Fe/H]+0.5; the metal abundance of the thick disk star is -3.0[Fe/H]+0.5, covering the metal abundance of the whole sample; the metallicity of the halo star is -3.0[Fe/H]-0.7., the thick disk and Bo Panheng star, the thick disk and the halo star, and the gold of the thin disk and the halo star. There are overlapping regions in the genus abundance, and three different star components can not be strictly distinguished from metallicity.
(2) average distribution of silver heart distance: R~m= 5.5~10.0 KPC of thin disk stars, mainly distributed in 7 ~9.0kpc; R~m= 4 ~ 11 KPC in thick disk stars, mainly distributed in the 5.5 ~7.5kpc range; R~m= 4 ~ 10 KPC of halo stars, mainly in the range of 4.5 ~6.0kpc. It also overlaps each other and can't be strictly differentiated.
(3) the maximum normal distance distribution: the maximum normal direction distance of the thin disk star in the vertical silver channel direction Z_ (max) 1kpc, the Z_ (max) =0.1 ~ 4kpc of the thick disk star, the Z_ (max) 1kpc. of the halo star, and the maximum normal distance between the thick disk and the thick disk, and the maximum normal distance between the thick disk and the halo star, and can not be strictly distinguished.
(4) the abundance of alpha elements (Mg, Si, Ca, Ti) [alpha /Fe] is relatively super abundant in poor metal stars, but the evolution trend of the 4 alpha elements is not completely consistent, and [the evolution trend of alpha /Fe] with metallicity [Fe/H] is also different in thin plates and thick disk stars. The abundance of 4 alpha elements in the thin disk stars [alpha /Fe] increases linearly with the increase of [Fe/H], to the increase of [Fe/H]. When the metal abundance of [Fe/H]=0 reaches the abundance of the solar system, [the increase of [alpha /Fe]] in the thick disk stars [alpha /Fe]=0.] is not monotonically decreasing, and the evolution of [Mg/Fe] is not exactly the same as the evolution of the other 3 kinds of alpha elements Si, Ca, Ti, and [Mg/Fe] in [Fe/H] -1.5 decreases linearly with the increase of [Fe/H]. ] = [Mg/Fe] between -2.0 and -0.7 is almost a platform distribution, but at the time of [Fe/H]-0.7, the [Mg/Fe] decreases rapidly with the increase of [Fe/H] to the abundance of the solar system, while the other 3 kinds of alpha elements, Si, Ca, and Ti [X/Fe] have been decreasing linearly with the increase of [Fe/H], but not in the entire metallicity range, but in [F. E/H] = -0.7 has a sudden drop in the "knee point", that is, [alpha /Fe] has a sudden acceleration drop with the increase of metallicity [Fe/H] to [Fe/H] = -0.7.
(5) in the overlapping region -1.0[Fe/H]+0.5 of thick disk and thin disk stellar metallicity, the [alpha /Fe]] between the thick disk star and the thin disk star is mixed together, and the thick disk and thin disk stars are not strictly divided according to the size of the alpha element abundances such as [Mg/Fe], but the average value of the thick disk stars [alpha /Fe] abundances is obviously higher than that of the thin disk stars.
(6) for the metal rich thin disk star ([Fe/H]0), the relative abundance of the 4 alpha elements, Si, Ca, Ti, [the evolution trend of the alpha /Fe] with the metallicity [Fe/H] is different: [Mg/Fe] continues to fall below the abundance of the solar system with the increase of [Fe/H]; [Si/Fe] and [Ca/Fe] are kept unchanged in the solar system when [Fe/H]0. A slight increase in the trend.
(7) [O/Fe] is consistent with the evolution trend of [Fe/H] with [Mg/Fe], but the [O/Fe] of thin disk star has a geniculate decline at [Fe/H] -0.4. [alpha /O] decreases linearly with the increase of [O/H], and [alpha /O] also exists in thin plates and thick plates, and can not be strictly differentiated, and the abundance of thick disc stars is larger than that of thin disc stars.
(8) the [alpha /Fe] abundances of the thick disk, the thin disk or the halo star are all related to the average orbital radius R~m of the star formation and the maximum distance Z_ (max) away from the silver channel, that is, there is no alpha abundance gradient. The alpha element abundances of the thin plates and the thick discs [alpha /Fe] are barely separated at R~m= 7kpc, but there are still some parts. The thick disk stars are mixed with thin disc stars; in the longitudinal direction of the silver disk, the alpha element abundances of the thin plates and the thick discs are separated at Z_ (max) =1kpc, but the same part of the thick disk star is also mixed in the thin disk region. The [alpha] /Fe] of the thick disk and the halo star can be distinctly separated in Z_ (max) =4kpc.
(9) the kinematic properties of the thin disk, the thick disk and the halo star are distinctly different, in which the difference in the velocity of the orbital velocity VLSR around the core is more obvious, the thin disk Star: V_ (LSR) -60km/s, and V_ (total) 90km/m; the thick disk Star: -180km/sV_ (LSR) -60km/s, and 250V_ (total) The velocity dispersion of the composition of the family is also different, and the velocity diffusion from the thin plate to the halo star increases in turn, but there is no correlation between the alpha abundance of the stars [alpha /Fe] and the kinematic velocity, and there are some stars with typical thin disk stars [alpha /Fe] abundance and kinematic thick disk, but also some typical thick disk stars [alpha]. /Fe] abundance in kinematics belongs to a thin disc star.
(10) the [alpha /Fe] abundance of the halo stars also decreases with the increase of [Fe/H], but the dispersion of the halo star is far greater than the analysis error of the abundance, and there is a serious mixture with the abundance of the alpha element in the thick disk star, and there are some [alpha /Fe] abundances below the thin plates as the poor alpha element halo stars. The [alpha /Fe] abundance of a thick disk star is higher than that of a thin disk star, but in the area of the metallicity overlap [alpha /Fe] is also intersecting with each other. It is not strictly differentiated. This is different from the observations of a single sample in recent years. Therefore, more large sample observations are needed for the distinction of the alpha element abundances of thin plates and thick disk stars. Confirmation.
【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】：2011
【分類號(hào)】：P144

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9 李霞;董雁冰;王亞輝;王俊;;空間光學(xué)輻射背景建模研究[A];2007年光電探測(cè)與制導(dǎo)技術(shù)的發(fā)展與應(yīng)用研討會(huì)論文集[C];2007年

10 王俊杰;;IRAS 04000-5052:恒星是怎樣在此形成的?(英文)[A];中國(guó)天文學(xué)會(huì)恒星分會(huì)2004年學(xué)術(shù)年會(huì)論文集[C];2004年

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