论文标题
SN 2014J的中间卵形相：集成作为重组的来源
The intermediate nebular phase of SN 2014J: onset of clumping as the source of recombination
论文作者
论文摘要
在大约1岁的时候，大多数IA型超新星的光谱以FEII和FEIII的强固性静脉发射线为主导。后来对附近SN 2011F的观察结果（约2年）显示了电离的意外转移向FEI和FEII。在此提出的中间阶段（1 - 1。5年）的附近SN IA 2014J的光谱显示出FEIII排放的逐渐下降，而FEI尚不强劲。如果至少在Fe为主导的区域中，射流中的团块的降低显着增加，则可以解释电离的减少。模型表明，大约一年后的团块保持连贯，表现得像弹片一样。团块中的高密度以及加热速率的降低将导致重组。这些数据可能见证了从相对平滑的射出到典型的SN残留物的非常块状形态的过渡阶段。增加结块的起源可能是局部磁场的发展。
At the age of about 1 year, the spectra of most Type Ia supernovae are dominated by strong forbidden nebular emission lines of FeII and FeIII. Later observations (at about 2 years) of the nearby SN 2011fe showed an unexpected shift of ionization to FeI and FeII. Spectra of the very nearby SN Ia 2014J at an intermediate phase (1 - 1.5 years) that are presented here show a progressive decline of FeIII emission, while FeI is not yet strong. The decrease in ionization can be explained if the degree of clumping in the ejecta increases significantly at ~1.5 years, at least in the Fe-dominated zone. Models suggest that clumps remain coherent after about one year, behaving like shrapnel. The high density in the clumps, combined with the decreasing heating rate, would then cause recombination. These data may witness the phase of transition from relatively smooth ejecta to the very clumpy morphology that is typical of SN remnants. The origin of the increased clumping may be the development of local magnetic fields.
