超冷矮星的长期多波长光变曲线：II。T2 .5 SIMP 0136的演变光变曲线和M9 TVLM 513的不相关光变曲线
Long-term, Multiwavelength Light Curves of Ultra-Cool Dwarfs: II. The evolving Light Curves of the T2.5 SIMP 0136 & the Uncorrelated Light Curves of the M9 TVLM 513
摘要：
我们提出了17个夜晚的可变L/T过渡褐矮星SIMP J013656.5+093347的地基，近红外测光和另外3个晚上的放射性晚M矮星TVLM 513-46546的地基测光。我们的TVLM 513-46546测光包括2个晚上的同时，多波长，地基测光，其中我们检测到明显的J波段变化，但没有检测到类似幅度的I波段变化，证实TVLM 513-46546的变化最有可能来自云或极光，而不是星点。我们对SIMP J013656.5+093347的测光包括15个夜晚的J波段测光，使我们能够观察这个L/T过渡褐矮星的可变光变曲线如何从旋转周期到旋转周期，从晚上到晚上和从星期到星期的演变。我们估计SIMP J013656.5+093347的自转周期为2.406 +/- 0.008小时，没有发现明显的差异自转的证据。SIMP J013656.5+093347在我们的光变曲线中显示的峰到峰幅度在几天内从大于6%演变到小于1%，SIMP J013656.5+093347光变曲线显著演变的典型时间尺度似乎约为<1到10个旋转周期。这表明，那些进行分光光度观测的褐矮星应该谨慎的解释比较光谱之间的一个变量褐矮星的最大流量和最小流量的观测持续只有大约一个旋转周期，因为这些比较可能描绘一个单一的光谱特征，短暂的快照，而不是完整的特征范围。
英文摘要：
We present 17 nights of ground-based, near-infrared photometry of the variable L/T transition brown dwarf SIMP J013656.5+093347 and an additional 3 nights of ground-based photometry of the radio-active late M-dwarf TVLM 513-46546. Our TVLM 513-46546 photometry includes 2 nights of simultaneous, multiwavelength, ground-based photometry, in which we detect obvious J-band variability, but do not detect I-band variability of similar amplitude, confirming that the variability of TVLM 513-46546 most likely arises from clouds or aurorae, rather than starspots. Our photometry of SIMP J013656.5+093347 includes 15 nights of J-band photometry that allow us to observe how the variable light curve of this L/T transition brown dwarf evolves from rotation period to rotation period, night-to-night and week-to-week. We estimate the rotation period of SIMP J013656.5+093347 as 2.406 +/- 0.008 hours, and do not find evidence for obvious differential rotation. The peak-to-peak amplitude displayed by SIMP J013656.5+093347 in our light curves evolves from greater than 6% to less than 1% in a matter of days, and the typical timescale for significant evolution of the SIMP J013656.5+093347 light curve appears to be approximately <1 to 10 rotation periods. This suggests that those performing spectrophotometric observations of brown dwarfs should be cautious in their interpretations comparing the spectra between a variable brown dwarf's maximum flux and minimum flux from observations lasting only approximately a rotation period, as these comparisons may depict the spectral characteristics of a single, ephemeral snapshot, rather than the full range of characteristics.
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