独特的星云相Ib型超新星2005 bf：一个可能的强磁化中子星诞生事件
The Unique Type Ib Supernova 2005bf at Nebular Phases: A Possible Birth Event of A Strongly Magnetized Neutron Star
摘要：
本文介绍了用斯巴鲁望远镜拍摄的Ib型超新星2005 bf在爆发后270天和310天的晚相星云光谱和测光结果。发射谱线（[OI]6300、6363、[CaII]7291、7324、[FeII]7155）显示蓝移约1，500 - 2，000 km s-1。[OI]双峰显示双峰曲线。线光度可以解释为来自一个只含有~ 0.1 - 0.4 Msun的团或喷流，其中~ 0.02 - 0.06 Msun是在爆炸时合成的56 Ni。为了解释蓝移现象，这个团状物应该是以质量中心速度v ~ 2，000 - 5，000 km s-1的单极运动，或者像SN 1990 I中看到的那样在喷出物中遭受自吸收。在这两种解释中，低质量团成分在第一个峰值（~ 20天）和后期阶段（~ 300天）都占主导地位。在后期阶段的低光度（在~ 270天的绝对R星等M_R ~ -10.2等）设定了56 Ni的质量上限< ~ 0.08 Msun，这与解释第二个主峰光度（在~ 40天的绝对R星等M_R ~ -18.3等）所需的值相矛盾。在56 Ni加热模型中遇到了这个困难，我们提出了一个替代方案，其中加热源是一个新诞生的强磁化中子星（磁星）的表面磁场Bmag ~ 10^{14-15}高斯和初始自旋周期P0 ~ 10 ms。然后，SN 2005 bf可以是正常SN e Ib/c和X射线闪光相关SN 2006 aj之间的链路，按照Bmag和/或P0连接。
英文摘要：
Late phase nebular spectra and photometry of Type Ib Supernova (SN) 2005bf taken by the Subaru telescope at ~ 270 and ~ 310 days since the explosion are presented. Emission lines ([OI]6300, 6363, [CaII]7291, 7324, [FeII]7155) show the blueshift of ~ 1,500 - 2,000 km s-1. The [OI] doublet shows a doubly-peaked profile. The line luminosities can be interpreted as coming from a blob or jet containing only ~ 0.1 - 0.4 Msun, in which ~ 0.02 - 0.06 Msun is 56Ni synthesized at the explosion. To explain the blueshift, the blob should either be of unipolar moving at the center-of-mass velocity v ~ 2,000 - 5,000 km s-1, or suffer from self-absorption within the ejecta as seen in SN 1990I. In both interpretations, the low-mass blob component dominates the optical output both at the first peak (~ 20 days) and at the late phase (~ 300 days). The low luminosity at the late phase (the absolute R magnitude M_R ~ -10.2 mag at ~ 270 days) sets the upper limit for the mass of 56Ni < ~ 0.08 Msun, which is in contradiction to the value necessary to explain the second, main peak luminosity (M_R ~ -18.3 mag at ~ 40 days). Encountered by this difficulty in the 56Ni heating model, we suggest an alternative scenario in which the heating source is a newly born, strongly magnetized neutron star (a magnetar) with the surface magnetic field Bmag ~ 10^{14-15} gauss and the initial spin period P0 ~ 10 ms. Then, SN 2005bf could be a link between normal SNe Ib/c and an X-Ray Flash associated SN 2006aj, connected in terms of Bmag and/or P0.
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