超冷矮星TVLM 513-46546的周期性射电和光学亮度变化的定时分析
Timing Analysis of the Periodic Radio and Optical Brightness Variations of the Ultracool Dwarf, TVLM 513-46546
摘要：
我们描述的到达时间测量和定时建模的周期性无线电耀斑和光学亮度变化的M9超冷矮星，TVLM 513-46546。我们确认了观测周期的稳定性，并确定其最佳拟合值为7054.468（+/-）0.007秒，在过去的7年中，基于新的和存档的无线电观测和存档的光学数据。当分别测量射电耀斑和光学周期时，周期相同，在（+/-）0.02秒内。我们表明，无线电耀斑的相位相对于光学亮度最大值由0.41（+/-）0.02的周期。我们的分析还表明，在较短的时间尺度上，周期随其长期平均值的（+/-）1-2 s的振幅而变化，并且这些变化与无线电波长和光波长之间相关。这些结果提供了进一步的证据，证明TVLM 513-46546配备了稳定的、近似偶极的磁场，该磁场为在宽波长范围内观察到的恒星活动提供动力，并且活动区域在不少于7年的时间里一直保持其身份和位置稳定性。根据2012年底和2013年初的阿雷西博射电望远镜定时观测，TVLM 513-46546的视射电耀斑周期逐步下降，这表明这种效应可能是恒星差异旋转的表现。
英文摘要：
We describe the arrival time measurements and timing modeling of the periodic radio flares and optical brightness variations of the M9 ultracool dwarf, TVLM 513-46546. We confirm the stability of the observed period and determine its best-fit value to be 7054.468(+/-)0.007 s over the last 7 years, based on both the new and archival radio observations and the archival optical data. The period, when measured separately for the radio flare and the optical periodicities, is the same to within (+/-)0.02 s. We show that the radio flares are out of phase with respect to the optical brightness maxima by 0.41(+/-)0.02 of the period. Our analysis also reveals that, on shorter timescales, the period varies with the amplitude of (+/-)1-2 s about its long-term average and that these variations are correlated between the radio and the optical wavelengths. These results provide further evidence that TVLM 513-46546 is equipped with a stable, approximately dipolar magnetic field which powers the activity of the star observed over a wide wavelength range, and that the active area has been maintaining its identity and positional stability over no less than 7 years. A stepwise decline of the apparent radio flaring period of TVLM 513-46546 deduced from timing observations with the Arecibo radio telescope in late 2012 and early 2013 suggests that this effect may be the manifestation of differential rotation of the star.
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