摘要
在中央中子星吸积模型较好地解释了超新星ＳＮ１９８７Ａ晚期光度演化的基础上，本文提出了ＳＮ１９８７Ａ晚期Ｘ射线辐射的一种新的解释．利用模型计算出的吸积光度以及ＳＮ１９８７Ａ膨胀气体包层的化学组分及分布，计算了出射的软Ｘ射线（０．５２ｋｅＶ）光度的演化，并与观测作了比较．我们认为ＳＮ１９８７Ａ晚期由中央中子星吸积产生的软Ｘ射线光度经过一段时间的增长后，将在４１００天左右开始下降．
Following the reasonable explanation of the evolution of the SN 1987A's bolometric luminosity at the later phase by the accretion model, we suggest that the observed soft X ray originates in the accretion of the central neutron star. Results of our model calculation are consistent with the observations. We predict that the observed X ray flux will increase only for a certain length of time, and will begin to decrease around day 4100.
基金
国家自然科学基金
