Astronomy and Astrophysics, volume 348, 877-887 (1999/8-3)
ISO spectroscopy of shocked gas in the vicinity of T Tauri.
VAN DEN ANCKER M.E., WESSELIUS P.R., TIELENS A.G.G.M., VAN DISHOECK E.F. and SPINOGLIO L.
Abstract (from CDS):
We present the results of ISO SWS and LWS spectroscopy of the young binary system T Tau. The spectrum shows absorption features due to H2O ice, CO2 ice, gas-phase CO and amorphous silicate dust, which we attribute to the envelope of T Tau S. We derive an extinction of AV=17.4mag±0.6mag towards this source. Detected emission lines from HI arise in the same region which is also responsible for the optical HI lines of T Tau N. These lines most likely arise in a partially ionized wind. Emission from the infrared fine-structure transitions of [SI], [ArII], [NeII], [FeII], [SiII], [OI] and [CII] was also detected, which we explain as arising in a ≃100km/s dissociative shock in a fairly dense (5x104cm–3) medium. Pure rotational and ro-vibrational emission from molecular hydrogen was detected as well. We show the H2 emission lines to be due to two thermal components, of 440 and 1500K respectively, which we attribute to emission from the dissociative shock also responsible for the atomic fine-structure lines and a much slower (≃35 km/s) non-dissociative shock. The 1500K component shows clear evidence for fluorescent UV excitation. Additionally, we found indications for the presence of a deeply embedded (AV>40m) source of warm H2 emission. We suggest that this component might be due to a shock, caused by either the outflow from T Tau S or by the infall of matter on the circumstellar disk of T Tau S.
stars: circumstellar matter - stars: individual: T Tau - stars: pre-main sequence - ISM: jets and outflows - infrared: stars
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