脉冲星辅助超新星遗迹中的尘埃形成
Dust formation in embryonic pulsar-aided supernova remnants
摘要：
研究了高能脉冲星风星云（PWNe）对尘埃形成和演化的影响。在许多超新星遗迹中也观测到尘埃排放，这些超新星遗迹也有中子星作为致密的遗迹。我们研究了尘埃形成时间和尘埃大小对喷出物和中心脉冲星性质的依赖关系。我们发现，脉冲星的初始自旋周期$P \sim 1\mbox{-}10\,\rm ms$和偶极磁场$B \sim 10^{12\mbox{-}15}\,\rm G$可以加速或延迟尘埃的形成，与几个月到十几年的时间尺度，并减少尘埃的平均大小的一个因素相比，非脉冲星的情况下$\sim$ 10或更多。我们还发现，在爆发后的2-5年内，在典型的超亮超新星中可以检测到$\sim$ 100-1000 Mpc的红外尘埃辐射，尽管这敏感地取决于星云非热辐射的光谱指数。我们讨论了以前的超新星观测的影响。尘埃形成模型和观测之间的一些差异，如SN 1987 A的形成时间或蟹状星云中的尘埃大小，可以用脉冲星的影响来解释，尘埃排放的知识对未来ALMA观测超亮超新星非常重要。
英文摘要：
We investigate effects of energetic pulsar wind nebulae (PWNe) on dust formation and evolution. Dust emission has been observed in many supernova remnants that also have neutron stars as compact remnants. We study the dependence of dust formation time and size on properties of the ejecta and central pulsar. We find that a pulsar with an initial spin period $P \sim 1\mbox{-}10\,\rm ms$ and a dipole magnetic field $B \sim 10^{12\mbox{-}15}\,\rm G$ can either accelerate or delay dust formation, with a timescale of several months to over ten years, and reduce the average size of dust by a factor of $\sim$ 10 or more compared to the non-pulsar case. We also find that infrared dust emission may be detectable in typical superluminous supernovae out to $\sim$ 100-1000 Mpc in 2-5 years after the explosion, although this depends sensitively on the spectral index of nonthermal emission from the nebula. We discuss implications to previous supernova observations. Some discrepancies between dust formation models and observations, such as the formation time in SN1987A or the dust size in the Crab Nebula, could be explained by the influence of a pulsar, and knowledge of the dust emission will be important for future ALMA observations of superluminous supernovae.
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