RW Aur A: SpeX Spectral Evidence for Differentiated Planetesimal Formation, Migration, and Destruction in an similar to 3 Myr Old Excited CTTS System

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 five different components: (1) a stable continuum from 0.7 to 1.3 mu m, with color temperature similar to 4000 K, produced by the CTTS photospheric surface; (2) variable hydrogen emission lines emitted from hot excited hydrogen in the CTTS's protostellar atmosphere/accretion envelope; (3) hot CO gas in the CTTS's protostellar atmosphere/accretion envelope; (4) highly variable 1.8-5.0 mu m thermal continuum emission with color temperature ranging from 1130 to 1650 K, due to a surrounding accretion disk that is spatially variable and has an inner wall at r similar to 0.04 au and T similar to 1650 K and outer edges at similar to 1200 K; and (5) transient, bifurcated signatures of abundant Fe ii + associated S i, Si i, and Sr i in the system's jet structures. The bifurcated signatures first appeared in 2015, but these collapsed and disappeared into a small single-peaked protostellar atmosphere feature by late 2020. The temporal evolution of RW Aur A's 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 a stable WTTS photospheric continuum from 0.7 to 1.3 mu m + cold CO gas in absorption + stable 1.8-5.0 mu m thermal disk continuum emission with color temperature similar to 1650 K.