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We present 2007 - 2020 SpeX VISNIR spectral monitoring of the highly variableRW Aur A CTTS. We find direct evidence for a highly excited, IR bright,asymmetric, and time variable system. Comparison of the spectral and temporaltrends found determines 5 different components: (1) a stable continuum from 0.7- 1.3 um, with approx color temperature 4000K, produced by the CTTSphotospheric surface; (2) variable hydrogen emission lines emitted from hotexcited hydrogen in the CTTSs protostellar atmosphere/accretion envelope; (3)hot CO gas in the CTTSs protostellar atmosphere/accretion envelope; (4) highlyvariable 1.8-5.0 um thermal continuum emission with color temperature rangingfrom 1130 to 1650K, due to a surrounding accretion disk that is spatiallyvariable and has an inner wall at r = 0.04 AU and T = 1650K, and outer edges atapprox 1200K; and (5) transient, bifurcated signatures of abundant Fe II +associated SI, SiI, and SrI in the systems jet structures. The bifuractedsignatures first appeared in 2015, but these collapsed and disappeared into asmall single peak protostellar atmosphere feature by late 2020. The temporalevolution of RW Aur As spectral signatures is consistent with a dynamicallyexcited CTTS system forming differentiated Vesta-sized planetesimals in anasymmetric accretion disk and migrating them inward to be destructivelyaccreted. 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 inabsorption + (4) stable 1.8-5.0 um thermal disk continuum emission with colortemperature approx 1650K.

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