RW Aur A：300万年前激发CTTS系统中有区别的星子形成、迁移和破坏的SpeX光谱证据
RW Aur A : SpeX Spectral Evidence for Differentiated Planetesimal Formation, Migration and Destruction in an 3 Myr Old Excited CTTS System
摘要：
我们提出了2007 - 2020年SpeX VISNIR光谱监测的高度可变RW Aur A CTTS。我们找到了直接的证据，一个高度兴奋，IR明亮，不对称，和时变系统。通过对谱线和时间趋势的比较，确定了5种不同的组分：（1）CTTS光球表面产生的0.7 - 1.3 μ m稳定连续谱，色温约为4000 K，（2）CTTS原恒星大气层/吸积包层中热激发氢的可变氢发射谱线，（3）CTTS原恒星大气层/吸积包层中热CO气体的可变氢发射谱线，（4）CTTS原恒星大气层/吸积包层中热CO气体的可变氢发射谱线，（5）CTTS原恒星大气层/吸积包层中热CO气体的可变氢发射谱线，（6）CTTS原恒星大气层/吸积包层中热CO气体的可变氢发射谱线。（4）由于周围的吸积盘是空间可变的，内壁在r = 0.04 AU，T = 1650 K，外缘在约1200 K，因此具有高度可变的1.8-5.0 μ m热连续谱发射，色温范围从1130 - 1650 K;（5）系统喷流结构中大量Fe Ⅱ +伴生的SI、SiI和SrI的瞬态分叉特征。分叉的签名首次出现在2015年，但到2020年底，这些签名崩溃并消失在一个小的单峰原恒星大气特征中。RW金作为光谱特征的时间演变是一致的动态激发CTTS系统形成分化灶神星大小的星子在一个不对称的吸积盘和迁移他们向内被破坏性吸积。相比之下，附近的同时期双星RW Aur B只显示出（1）稳定的0.7 - 1.3 μ m的WTTS光球连续谱+（3）吸收中的冷CO气体+（4）稳定的1.8-5.0 μ m的热盘连续谱发射，色温约为1650 K。
英文摘要：
We present 2007 - 2020 SpeX VISNIR spectral monitoring of the highly variable RW Aur A CTTS. We find direct evidence for a highly excited, IR bright, asymmetric, and time variable system. Comparison of the spectral and temporal trends found determines 5 different components: (1) a stable continuum from 0.7 - 1.3 um, with approx color temperature 4000K, produced by the CTTS photospheric surface; (2) variable hydrogen emission lines emitted from hot excited hydrogen in the CTTSs protostellar atmosphere/accretion envelope; (3) hot CO gas in the CTTSs protostellar atmosphere/accretion envelope; (4) highly variable 1.8-5.0 um thermal continuum emission with color temperature ranging from 1130 to 1650K, due to a surrounding accretion disk that is spatially variable and has an inner wall at r = 0.04 AU and T = 1650K, and outer edges at approx 1200K; and (5) transient, bifurcated signatures of abundant Fe II + associated SI, SiI, and SrI in the systems jet structures. The bifuracted signatures first appeared in 2015, but these collapsed and disappeared into a small single peak protostellar atmosphere feature by late 2020. The temporal evolution of RW Aur As spectral signatures is consistent with a dynamically excited CTTS system forming differentiated Vesta-sized planetesimals in an asymmetric accretion disk and migrating them inward to be destructively accreted. By contrast, nearby, coeval binary companion RW Aur B evinces only (1) a stable WTTS photospheric continuum from 0.7 - 1.3 um + (3) cold CO gas in absorption + (4) stable 1.8-5.0 um thermal disk continuum emission with color temperature approx 1650K.
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