多方气体球引力坍缩中激波的形成和传播

本文采用计算流体力学中的高分辨率ＰＰＭ格式，数值模拟了多方气体球的引力坍缩、激波形成和传播。物态方程取成ｐ＝Ｋ（ｓ）ρ＾γ，γ为密度的分段函数，通过绝热指数γ的不同取法对三个模型分别进行了计算，并对引力坍缩、反弹激波形成和传播等三个过程及不型之间计算结果的一些差异做了比较仔细的分析，得到了一些初步结论。     

辐射能耗对激波传播的影响

我们对激波传播的前期,以绝热解为基础,建立了辐射能耗对传播影响的一级微扰方程。若对传播后期采用无驱动近似,我们重新建立了等效分界时刻的定义标准。把前期作为绝热传播的方法与本方法比较表明,前者的结果比后者大若干倍。     

超新星爆发的前身星模型研究

本利用Ｗｏｏｓｌｅｙ提供的４个不同的前身星模型数据作为计算的前超新星分布，并利用自己独立编制的程序和改进的状态方程进行数值模拟。对其结果进行分析比较，考察前身星对超新星的坍缩、激波传输和爆发等过程的影响。     

Ia型超新星“SN2013gt”发现记

不知道从什么时候,我开始喜欢上了在没有色彩的星系图片中搜寻未知的星星。     

Quark-Novae Ia in the Hubble diagram: implications for dark energy

The accelerated expansion of the Universe was proposed through the use of Type-Ia supernovae （SNe） as standard candles. The standardization depends on an empirical correlation between the stretch/color and peak luminosity of the light curves. The use of Type-Ia SNe as standard candles rests on the assumption that their properties （and this correlation） do not vary with redshift. We consider the possibility that the majority of Type-Ia SNe are in fact caused by a Quark-Nova detonation in a tight neutron-star-CO-white-dwarf binary system, which forms a Quark-Nova Ia （QN-Ia）. The spin-down energy injected by the Quark-Nova remnant （the quark star） contributes to the post-peak light curve and neatly explains the observed correlation between peak luminosity and light curve shape. We demonstrate that the parameters describing QN-Ia are NOT constant in redshift. Simulated QN-Ia light curves provide a test of the stretch/color correlation by comparing the true distance modulus with that determined using SN light curve fitters. We determine a correction between the true and fitted distance moduli, which when applied to Type-Ia SNe in the Hubble diagram recovers the ΩM = 1 cosmology. We conclude that Type-Ia SNe observations do not necessitate the need for an accelerating expansion of the Universe （if the observed SNe Ia are dominated by QNe Ia） and by association the need for dark energy.