超核密度壓縮參數(shù)對Ⅱ型超新星爆發(fā)的影響
[Abstract]:In this paper, by using the data of the predecessor star model provided by Woosley in 2002 and the program "SHII-WLYW89", we calculate the supernovae whose predecessor stars are 11m _ (?), () ~ (13) M _ (?), (15M), 20m _ (?), 25M _ (?), 30M _ (?), 35M _ (?), 40m _, and adjust the parameters v in the equation of state. The effects of v on the collapse of supernova star nucleus, the propagation of shock wave and the burst energy in the equation of state are discussed, which will provide the basis for the improvement of the equation of state. The results show that: 1. At the stage of star collapse, the value of YLc,Yec,Yvc remains unchanged with the increase of v, but the entropy of the center decreases and the value of pmaxc is smaller, that is, the equation of state is softer; 2. In the process of rebound, the higher v value, the larger the EvH, that is, the greater the energy of neutrino walking. However, the total binding energy of mass kinetic energy, internal energy and gravitational potential energy in the same mode region (the energy transferred from the core to the outer nucleus between t 4 and t 11) increases first and then decreases with the increase of v. In comparison, for different masses of precursors, the v value of the inner star's nucleus transferring to the maximum of the energy of the alien nucleus is not the same as that of the former star's. 3. 3. Under the four-particle model, when we investigate the effect of v variation on the burst energy of different solar mass models, we find that the best compression parameters of supernuclei density are different for different solar mass models. The results showed that vx2 was more suitable; These results indicate that v has an important effect on the collapse of supernova iron nuclei, energy transfer at shock wave propagation time and burst energy. This is of great significance for the study of supernova eruptions.
【學(xué)位授予單位】:廣西師范大學(xué)
【學(xué)位級別】:碩士
【學(xué)位授予年份】:2011
【分類號】:P145.3
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