F. Lopez-Martinez, J. F. Gameiro
Abstract
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 ≤ logTe (K) ≤ 4.55 and 2.25 ≤ logne (cm3) ≤ 5.25 and another one with 5.25 ≤ logTe (K) ≤ 5.6 and 5.25 ≤ logne (cm3) ≤ 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.
JET Simulations, Experiments, and Theory
C. Sauty
Springer Nature
ASSSP
Volume 55, Page 97
2019 August
