Analysis of the Physical Properties of Jets/Outflows in T Tauri Stars

Winds and jets are key factors in the evolution of accreting young stellar objects. For a full understanding of the connection among outflows, jets and the accretion processes, it is important a reliable determination of their physical properties. In this work we used the theoretical [N II], [O I] and [S II] flux ratios to derive the high velocity component (HVC) and low velocity component (LVC) of T Tauri outflow/jet properties where these lines are formed. We found two well-defined ranges of temperatures and densities for the emitting region: one with \(4.125 \leq \log T_{\mathrm {e}}\mathrm {(K)} \leq 4.55\) and \(2.25 \leq \log n_{\mathrm {e}}(\mathrm {cm}^3) \leq 5.25\) and another one with \(5.25 \leq \log T_{\mathrm {e}}\mathrm {(K)} \leq 5.6\) and \(5.25 \leq \log n_{\mathrm {e}}(\mathrm {cm}^3) \leq 6.75\). Peak velocities and full width at half maximum of the LVC point out that its origin is from a MHD disk wind at 0.05–1.69 AU from the source and that the lines are broadened by Keplerian rotation.