本文選題：密近雙星 + 恒星演化　； 參考：《新疆大學(xué)》2015年碩士論文

【摘要】：紅新星由于其特殊的光譜和光度特性一直備受關(guān)注。V1309 Sco和V838 Mon的觀(guān)測(cè)數(shù)據(jù)表明這類(lèi)恒星很可能是由雙星合并產(chǎn)生的。如果是這樣,那么紅新星的研究就給我們認(rèn)識(shí)雙星的合并提供了一種新的途徑。假定紅新星起源于雙星合并,并結(jié)合紅新星的觀(guān)測(cè)數(shù)據(jù),本文對(duì)紅新星做了一個(gè)細(xì)致的研究。首先,根據(jù)紅新星的觀(guān)測(cè)特性,我們分析和擬合了光度和溫度隨時(shí)間的演化。其次,我們給出了V1309 Sco,V838 Mon以及初始質(zhì)量在1 M⊙到40 M⊙之間的普通恒星在赫羅圖中的演化,并對(duì)它們的演化軌跡進(jìn)行比較。我們發(fā)現(xiàn)紅新星的演化與普通恒星的演化完全不同。紅新星最終演化成一顆Hayashi線(xiàn)附近的恒星。紅新星的質(zhì)量等于其前身星系統(tǒng)中雙星的總質(zhì)量。并且如果紅新星的質(zhì)量與一個(gè)零齡主序星的質(zhì)量相同,那么紅新星和這顆主序星會(huì)演化到相同的Hayashi線(xiàn)附近。再次,利用星族合成的方法,我們估算了銀河系紅新星的誕生率。我們得出紅新星在銀河系中的誕生率為0.14 yr-1。其中大約有62%的紅新星來(lái)自于紅巨星和主序星的合并,大約22%的紅新星起源于白矮星和主序星合并,大約11%的紅新星起源于Hertzsprung間隙的恒星和主序星的合并,大約有3%的紅新星來(lái)自于主序星和主序星的合并,其余的雙星合并忽略。最后,我們還研究了紅新星前身星系統(tǒng)的一些性質(zhì)。我們發(fā)現(xiàn)紅新星前身星系統(tǒng)中主星主要為小質(zhì)量的恒星,軌道周期大約為2~62天。
[Abstract]:The observational data of V1309 Sco and V838 Mon indicate that the red nova is probably produced by the combination of binary stars due to its special spectral and photometric properties. If so, the study of Red Nova offers a new way to understand the combination of binary stars. Assuming that the red nova originated from the combination of binary stars and combined with the observational data of the red nova, this paper makes a detailed study of the red nova. Firstly, according to the observed characteristics of the red nova, we analyze and fit the evolution of luminosity and temperature with time. Secondly, we give the evolution of V1309 Scot V838 Mon and ordinary stars with initial mass from 1m to 40 M _ (298) in the Hero diagram, and compare their evolution trajectories. We find that the evolution of red novae is completely different from that of ordinary stars. The red nova eventually evolved into a star near the Hayashi line. The mass of a red nova is equal to the total mass of a binary star in its predecessor star system. And if the mass of the red nova is the same as that of a zero-age principal sequence star, then the red nova and the principal sequence star will evolve to the same Hayashi line. Thirdly, we estimate the birth rate of galactic red nova by the method of star family synthesis. We find that the birth rate of red nova in the Milky way is 0. 14 yr-1. About 62% of the red novae come from the combination of the red giant and the main sequence star, about 22% of the red novae originate from the combination of the white dwarf star and the principal sequence star, and about 11% of the red novae originate from the merging of stars and principal sequence stars in the Hertzsprung gap. About 3% of the red novae come from the combination of the principal sequence star and the principal sequence star, while the remaining binary stars are ignored. Finally, we study some properties of the red nova precursor star system. We find that the main star in the precursor system of red nova is mainly a small mass star with an orbital period of about 2 ~ 62 days.
【學(xué)位授予單位】：新疆大學(xué)
【學(xué)位級(jí)別】：碩士
【學(xué)位授予年份】：2015
【分類(lèi)號(hào)】：P144

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