【摘要】：超新星爆發(fā)是宇宙最激烈的天體物理現(xiàn)象之一，是某些恒星演化到生命的最后階段的爆發(fā)性的終結(jié)，釋放出大量的物質(zhì)和極高的能量。超新星依據(jù)其光譜中有無(wú)氫線，分為II型和I型，沒(méi)有氫線的I型又分為Ia、Ib和Ic。超新星的宿主星系，也就是超新星的爆發(fā)環(huán)境，對(duì)超新星的爆發(fā)有重要的影響，已經(jīng)有很多工作研究了不同金屬豐度、不同年齡的宿主星系中超新星爆發(fā)的類型及特征等。 PrantzosBoissier（2003）和BoissierPrantzos（2009）曾研究發(fā)現(xiàn)超新星Ibc與II的數(shù)目比值隨宿主星系金屬豐度的增加而增大，并認(rèn)為其結(jié)果與有旋轉(zhuǎn)的大質(zhì)量星的演化模型相一致； Preito et al.（2008）通過(guò)直接測(cè)定超新星宿主星系整體的金屬豐度，發(fā)現(xiàn)超新星Ibc的宿主星系比Ia和II的顯示出更高的金屬豐度；Hammuy etal.（1996）發(fā)現(xiàn)內(nèi)稟暗的事件發(fā)生在早型星系中，而亮的事件發(fā)生在晚型的宿主星系中； Gallagher et al.（2008）認(rèn)為發(fā)生在年齡較老星系中的超新星Ia的峰值光度比更年輕星系中的超新星Ia暗約一個(gè)星等，即更暗的超新星Ia發(fā)生在更老星族的星系中；Sullivan et al.（2006）Aubourg et al.（2008）發(fā)現(xiàn)超新星Ia宿主星系中短壽命前身星星族的證據(jù)，對(duì)超新星Ia的前身星質(zhì)量范圍給出了一定的限制。雖然已經(jīng)有這些研究結(jié)果，但他們基于的樣本一般都比較小，特別是還沒(méi)有對(duì)SN Ia、II、Ib/c幾種不同類型超新星宿主星系的星族進(jìn)行詳細(xì)比較的工作，而星族是表征超新星爆發(fā)環(huán)境的一個(gè)非常重要的直接參量，因此我們將SDSS主星系表與Asiago超新星表進(jìn)行交叉，選出234個(gè)不同類型超新星及其宿主星系，詳細(xì)分析了他們的星族成分。 我們利用30arcsec的交叉半徑，對(duì)SDSS主星系表和Asiago超新星表中宿主星系的坐標(biāo)進(jìn)行了交叉，將得到的1201個(gè)樣本，隨后又以light-fraction0.15為衡量標(biāo)準(zhǔn)進(jìn)一步取了一個(gè)次樣本，其3角秒的fiber觀測(cè)光譜能較好的表征星系整體光的性質(zhì)。之后更進(jìn)一步檢查了樣本的圖像和光譜觀測(cè)，最終得到234個(gè)星系，分為兩類進(jìn)行研究分析：137個(gè)發(fā)射線星系和97個(gè)吸收線星系。 對(duì)這兩類星系，我們用STARLIGHT擬合了連續(xù)譜和吸收線，得到了他們不同年齡和不同金屬豐度的星族成分，并從MPA/JHU數(shù)據(jù)庫(kù)中得到Dn (4000)、H A、恒星質(zhì)量、恒星形成率等特征參量，對(duì)超新星Ia、II、Ib/c三種類型超新星宿主星系的特征結(jié)果進(jìn)行了比較分析。然后，對(duì)于137個(gè)發(fā)射線星系，又利用MPA/JHU團(tuán)組提供的H和H的等值寬度，計(jì)算了星系中年輕星族的年齡。通過(guò)分析我們發(fā)現(xiàn)： 對(duì)于發(fā)射線星系樣本，1）SN II宿主星系的年輕星族成分貢獻(xiàn)最大，表明他們比SN Ia和Ib/c宿主星系更年輕，SN Ia宿主星系比SN Ib/c宿主星系稍微年輕一點(diǎn)；2）SN II宿主星系的富金屬星族成分貢獻(xiàn)最少，SN Ib/c宿主星系的富金屬星族成分貢獻(xiàn)最大，SN Ia位于二者之間，，表明SN Ib/c比SN II爆發(fā)在相對(duì)更加富金屬的環(huán)境中；3）通過(guò)Hα和Hβ發(fā)射線等值寬度估計(jì)出的宿主星系年輕星族的年齡，給出了超新星爆發(fā)環(huán)境的年齡下限；4）SN Ia傾向于爆發(fā)在大質(zhì)量的星系內(nèi)，SN II爆發(fā)在大質(zhì)量和中小質(zhì)量的星系內(nèi)。 對(duì)于吸收線星系樣本，1）SN Ia宿主星系的年輕星族成分貢獻(xiàn)最小，老年星族成分貢獻(xiàn)最大，表明他們比SN Ib/c和II宿主星系更年老；2）SN Ia宿主星系的富金屬星族成分貢獻(xiàn)最大，表明其爆發(fā)在相對(duì)富金屬的環(huán)境中。 對(duì)比發(fā)射線星系和吸收線星系，1）對(duì)同種類型超新星，發(fā)射線宿主星系的年輕星族成分更多，比吸收線宿主星系更年輕；2）對(duì)同種類型超新星，吸收線宿主星系比發(fā)射線宿主星系更加富金屬；3）吸收線宿主星系的恒星質(zhì)量相對(duì)較大，恒星形成率相對(duì)較低。
[Abstract]:The supernova eruption is one of the most intense astrophysical phenomena in the universe. It is the explosive end of the last stage of the evolution of some stars to life. It releases a lot of material and high energy. Supernova is divided into II and I based on its hydrogen free line in its spectrum. The I type without hydrogen line is also divided into host galaxies of Ia, Ib and Ic. supernova, too. The outbreak of supernova has an important impact on the outbreaks of supernovae. Many work has been done to study the types and characteristics of supernova eruptions in host galaxies of different metallicity and age.
PrantzosBoissier (2003) and BoissierPrantzos (2009) have found that the ratio of the number of supernova Ibc to II increases with the increase in the metallicity of the host star system, and considers that the result is in accordance with the evolution model of the large mass star with rotation; Preito et al. (2008) detected the metallicity of the whole supernova host galaxy by direct connection. The host galaxies of supernova Ibc showed higher metallicity than Ia and II; Hammuy etal. (1996) found that the intrinsic dark events occurred in the early type galaxies, and the bright events occurred in the late type host galaxy; Gallagher et al. (2008) believed that the peak luminosity of the supernova Ia in the older stars was younger than the younger galaxy. The supernova Ia is dark about one star, that is, the darker supernova Ia occurs in the older star galaxy; Sullivan et al. (2006) Aubourg et al. (2008) finds the evidence of the short life precursor star in the supernova Ia host galaxy, which limits the mass range of supernova Ia's precursor. Although these results have been found, However, the samples they are based on are generally relatively small, especially for the SN Ia, II, Ib/c and different types of supernova host galaxies in detail, and the star family is a very important direct parameter to characterize the supernova environment, so we cross the SDSS star table with the Asiago supernova table. Two hundred and thirty-four different types of supernovae and their host galaxies were analyzed in detail.
Using the cross radius of 30arcsec, we cross the coordinates of the host galaxy table of SDSS and the host galaxy in the Asiago supernova table. 1201 samples are obtained, and then a sub sample is taken by light-fraction0.15 as a measure. The fiber view spectrum of the 3 corner seconds can better characterize the properties of the whole galaxy light. Further examination of the image and spectral observations of the samples, and finally get 234 galaxies, divided into two types of research and analysis: 137 emitter galaxies and 97 absorption line galaxies.
For these two types of galaxies, we use STARLIGHT to fit the continuous spectrum and absorption line, get their different age and different metallicity, and get Dn (4000), H A, stellar mass and star formation rate from the MPA/JHU database, and carry out the characteristics of the supernova Ia, II, Ib/c, three types of supernova host galaxies. Then, for 137 emission line galaxies, we use the equivalent widths of H and H provided by the group of MPA/JHU groups to calculate the age of the middle age light stars in the galaxy.
For the emission line Galaxy samples, 1) the young star composition of the SN II host galaxy contributes the most, indicating that they are younger than the SN Ia and Ib/c host stars, and the SN Ia host galaxy is a little younger than the SN Ib/c host star system; and the SN II host galaxy has the least contribution to the rich metallic star component, and the rich metallic star component of the SN main star system contributes the most. Large, SN Ia is between two, indicating that SN Ib/c outbreaks in a relatively more metal rich environment than SN II; 3) the age of the young star family of the host galaxy estimated by the H alpha and H beta emission line equal width, gives the age limit of the supernova explosion environment; 4) SN Ia tends to explode in mass galaxies, SN II erupts in mass and Small and medium galaxies.
For the sample of the absorption line galaxies, 1) the young star composition of the SN Ia host galaxy has the smallest contribution to the young star family component, and the older star composition contributes most, indicating that they are older than the SN Ib/c and the II host galaxies; 2) the rich metallic star component of the SN Ia host galaxy contributes the most, indicating that its eruption is in the relatively metal rich environment.
Compared with the emitter and absorption line galaxies, 1) for the same type supernova, the young star family of the host galaxy is more, younger than the absorption line host star system; 2) for the same type supernova, the absorption line host star system is more metal than the ray host galaxy; 3) the star mass of the absorption line host galaxy is relatively large, and the star is relatively large. The formation rate is relatively low.
【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】：2012
【分類號(hào)】：P152

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