红新星的研究

发布时间：2018-05-24 11:48

本文选题：密近双星 + 恒星演化　；参考：《新疆大学》2015年硕士论文

【摘要】：红新星由于其特殊的光谱和光度特性一直备受关注。V1309 Sco和V838 Mon的观测数据表明这类恒星很可能是由双星合并产生的。如果是这样,那么红新星的研究就给我们认识双星的合并提供了一种新的途径。假定红新星起源于双星合并,并结合红新星的观测数据,本文对红新星做了一个细致的研究。首先,根据红新星的观测特性,我们分析和拟合了光度和温度随时间的演化。其次,我们给出了V1309 Sco,V838 Mon以及初始质量在1 M⊙到40 M⊙之间的普通恒星在赫罗图中的演化,并对它们的演化轨迹进行比较。我们发现红新星的演化与普通恒星的演化完全不同。红新星最终演化成一颗Hayashi线附近的恒星。红新星的质量等于其前身星系统中双星的总质量。并且如果红新星的质量与一个零龄主序星的质量相同,那么红新星和这颗主序星会演化到相同的Hayashi线附近。再次,利用星族合成的方法,我们估算了银河系红新星的诞生率。我们得出红新星在银河系中的诞生率为0.14 yr-1。其中大约有62%的红新星来自于红巨星和主序星的合并,大约22%的红新星起源于白矮星和主序星合并,大约11%的红新星起源于Hertzsprung间隙的恒星和主序星的合并,大约有3%的红新星来自于主序星和主序星的合并,其余的双星合并忽略。最后,我们还研究了红新星前身星系统的一些性质。我们发现红新星前身星系统中主星主要为小质量的恒星,轨道周期大约为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.
【学位授予单位】：新疆大学
【学位级别】：硕士
【学位授予年份】：2015
【分类号】：P144

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