论文标题
RW AUR A：SPEX光谱证据，证明了3 Myr旧激发CTTS系统中分化的行星形成，迁移和破坏
RW Aur A : SpeX Spectral Evidence for Differentiated Planetesimal Formation, Migration and Destruction in an 3 Myr Old Excited CTTS System
论文作者
论文摘要
我们提出了2007年至2020年的SPEX Visnir光谱监测，对高度可变的RW AUR A CTTS。我们发现直接证据表明非常激发，ir亮，不对称和时间变量系统。发现的光谱和时间趋势的比较确定了5个不同的组成部分：（1）CTTS Photompheric表面产生的0.7-1.3 um的稳定连续体稳定的连续体。 （2）CTTSS Protostellar气氛/增生包膜中从热激发氢发出的可变氢发射线； （3）CTTSS原始大气中的热CO气体/积聚包膜； （4）高度可变的1.8-5.0 um热连续性发射，色温范围为1130至1650k，这是由于周围的积聚磁盘在空间上可变，内壁在r = 0.04 au和t = 1650k的内壁，外边缘约为1200k； （5）系统射流结构中大量的Fe II +相关SI，SII和SRI的瞬时，分叉的特征。 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.相比之下，附近的同时二进制伴侣RW AUR仅证明了（1）稳定的WTTS光球连续体，吸收吸收中的0.7-1.3 um +（3）冷Co气体 +（4）稳定的1.8-5.0 um热盘连续性发射，颜色温度约为1650k。
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.
