本文選題：郭守敬望遠(yuǎn)鏡 + 金屬豐度分布函數(shù)　； 參考：《上海師范大學(xué)》2015年碩士論文

【摘要】：研究銀河系矮星的金屬豐度分布函數(shù)(MDF)對理解銀河系化學(xué)演化和動力學(xué)演化有重要意義。像F、G、K型矮星這樣的冷星的年齡,被認(rèn)為大于或者相當(dāng)于銀盤的年齡。所以,曾經(jīng)誕生于銀河系中的這些恒星都還沒有離開主序階段。通過測量和研究這些冷星的金屬豐度分布函數(shù),可以為盤星的形成歷史及其演化提供嚴(yán)格的約束。當(dāng)然,比G矮星更冷的恒星,比如K矮星或者M(jìn)矮星有比G矮星更長的壽命。然而,鑒于這些恒星光度較小,基于K矮星或M矮星的樣本可能僅僅在一個小的區(qū)域內(nèi),同時,還會有更多的偏差,更難得到一個無偏的、完備的樣本。大天區(qū)面積多目標(biāo)光纖光譜望遠(yuǎn)鏡(LAMOST,又稱為郭守敬望遠(yuǎn)鏡)可以在一次曝光中同時得到4000個目標(biāo)天體的低分辨率光譜。郭守敬望遠(yuǎn)鏡具有20平方度的視場,同時具有3.6-4.9m的有效通光半徑。此巡天觀測有兩個觀測計劃:河外星系巡天(LEGAS)和旨在研究銀河系結(jié)構(gòu)的銀河系巡天(LEGUE)兩部分。我們的研究目標(biāo)是基于郭守敬望遠(yuǎn)鏡銀河系巡天研究太陽附近G矮星的金屬豐度分布函數(shù)。我們從LAMOST DR2中選出太陽附近的282,217顆G矮星,并研究其金屬豐度分布函數(shù)。然后,將我們得到的基于LAMOST銀河系巡天的G矮星的金屬豐度分布函數(shù)與源自日內(nèi)瓦-哥本哈根(GCS)太陽附近的研究(一個星等完備,運動學(xué)上無偏的近鄰的16,682顆F和G矮星樣本)得到的測光較好的irfm樣本作比較。我們發(fā)現(xiàn),與GCS樣本相比,我們的樣本有更高比例的貧金屬星。最后,我們認(rèn)為,當(dāng)我們基于LAMOST光譜巡天研究太陽附近G矮星的金屬豐度分布函數(shù)時,可能存在選擇效應(yīng)。
[Abstract]:The study of the metal abundance distribution function (MDF) of the Milky way Dwarfs is of great significance in understanding the chemical and kinetic evolution of the Milky way. Cold stars such as the FGG K dwarf are believed to be older than or equal to the silver disk. So the stars that were born in the Milky way haven't left the main sequence yet. By measuring and studying the metal abundance distribution function of these cold stars, it is possible to provide strict constraints for the formation history and evolution of these cold stars. Of course, stars colder than G dwarfs, such as K dwarfs or M dwarfs, have longer lifetimes than G dwarfs. However, given the small luminosity of these stars, samples based on K or M dwarfs may only be in a small region, and at the same time, there will be more deviations and it will be more difficult to obtain an unbiased, complete sample. LAMOST (also known as Guo Shoujing Telescope) can obtain the low resolution spectra of 4,000 target objects in a single exposure at the same time. The Kuo Shoujing telescope has a field of view of 20 square degrees and an effective radius of 3.6-4.9 m. There are two observational plans for this survey: the Extragalactic Survey (LEGASS) and the Galactic Profiler (LEGUE) to study the structure of the Milky way. Our aim is to study the metal abundance distribution function of G dwarf stars near the Sun based on the Galactic Survey of the Kuo Shoujing Telescope. We select 282217 G dwarfs from LAMOST DR2 and study their metal abundance distribution function. Then, the metal abundance distribution function of the G dwarf star based on the LAMOST Galaxy Survey and the study near the Sun from the Geneva-Copenhagen GCSs (a magnitude complete) are obtained. 16682 samples of F and G dwarfs with unbiased kinematics are compared with irfm samples with better photometry. We found that our sample has a higher proportion of poor metal stars than the GCS sample. Finally, we consider that there may be a selective effect when we study the metal abundance distribution function of G dwarf stars near the sun based on the LAMOST spectral survey.
【學(xué)位授予單位】：上海師范大學(xué)
【學(xué)位級別】：碩士
【學(xué)位授予年份】：2015
【分類號】：P148

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本文編號：2018965