摘要
超新星ＳＮ１９８７Ａ中央可能存在的致密天体（如中子星），通过吸积那些超新星爆发时抛射速度小于逃逸速度的物质而产生的吸积光度，对ＳＮ１９８７Ａ晚期的热光度演化有重要的贡献．本文改进了以前的理论模型，给出了更为合理的定量计算，对所提出的特殊的吸积机制作出了仔细分析，特别强调，这种吸积是膨胀包层中的物质由于引力作用引起的长时期内的连续回落，它有别于其它的吸积模型，并给出直接的观测证据．假设致密天体是１４Ｍ⊙，半径为１０６ｃｍ的中子星，我们的计算表明，它的吸积能提供足够的能量来形成ＳＮ１９８７Ａ热光度曲线在１０５０天左右时的鼓包。
he investigations of the bolometric light curve of SN 1987A are briefly reviewed. We suggest that the accretion luminosity produced by an assumed neutron star at the center of SN 1987A is important for the late evolution of the bolometric light curve. We emphasize the marked difference between our consideration and the previous accretion models, where the backfall of material occurs primarily within the first few seconds after explosion and the details of accretion are dependent on the explosion mechanism which is very uncertain. In this paper, we are concerned with the continuous gravitational infall of material within the expansion envelope. Our suggestion is directly inspired by the line-profile observations and is only weakly dependent on the explosion model. Taking the values of a typical neutron star as r*=106 cm and M*=14M⊙, the model calculation fits the observed light curve well. This in turn supports the assumption of the presence of a central neutron star.
基金
国家自然科学基金
