论文标题
RW AUR A的射流弹出和质量积聚之间可能的时间相关
Possible Time Correlation Between Jet Ejection and Mass Accretion for RW Aur A
论文作者
论文摘要
对于活跃的T-Taur Star RW AUR A，我们使用Gemini-Nifs和VLT-Sinfoni进行了[Fe II] 1.644微米发射线（1）喷气成像的长期（〜10年）监测观察结果； （2）使用CFHT-ESPADON的光学高分辨率光谱； （3）使用CRAO 1.25 m望远镜和AAVSO的V波段光度法。后两个观察结果证实了（a）Ca II 8542 A和O I 7772之间的时间变化的相关性，与磁层积聚相关的线曲线以及（b）光学连续元素通量。喷射图像及其适当的动作表明，在过去的15年中，恒星发生了四个结弹出，不规则间隔为2 - 6年。这些间隔的时间尺度和不规则性与光学光度计数据中看到的调光事件的时间尺度和不规则性相似。我们的观察结果显示了显着（Delta_v <-1 mag。）光度升高和喷射结弹出之间的可能联系。在另外几年中的观察可能会证实或拒绝这一趋势。如果得到确认，这将暗示喷气发射区的位置非常接近恒星（R << 0.1 AU），如某些喷气式发射型号所预测。这样的结论对于理解恒星的几个AU中的磁盘进化至关重要，因此在这些半径上可能持续的行星形成。
For the active T-Taur star RW Aur A we have performed long-term (~10 yr) monitoring observations of (1) jet imaging in the [Fe II] 1.644-micron emission line using Gemini-NIFS and VLT-SINFONI; (2) optical high-resolution spectroscopy using CFHT-ESPaDOnS; and (3) V-band photometry using the CrAO 1.25-m telescope and AAVSO. The latter two observations confirm the correlation of time variabilities between (A) the Ca II 8542 A and O I 7772 A line profiles associated with magnetospheric accretion, and (B) optical continuum fluxes. The jet images and their proper motions show that four knot ejections occurred at the star over the past ~15 years with an irregular interval of 2-6 years. The time scale and irregularity of these intervals are similar to those of the dimming events seen in the optical photometry data. Our observations show a possible link between remarkable (Delta_V < -1 mag.) photometric rises and jet knot ejections. Observations over another few years may confirm or reject this trend. If confirmed, this would imply that the location of the jet launching region is very close to the star (r <<0.1 au) as predicted by some jet launching models. Such a conclusion would be crucial for understanding disk evolution within a few au of the star, and therefore possible ongoing planet formation at these radii.
