Emission lines from rotating proto-stellar jets with variable velocity profiles

I. Three-dimensional numerical simulation of the non-magnetic case

¹ LATO-DCET-UESC, Rodovia Ilhéus-Itabuna km 16, Ilhéus, Bahia, 45662-000, Brazil e-mail: [hoth;mjvasc]@uesc.br
² Instituto de Ciencias Nucleares, UNAM, Ap. Postal 70-543, CU, D.F., 04510, México e-mail: [pablo;raga]@nucleares.unam.mx
³ Instituto de Astronomía, UNAM, Ap. Postal 70-543, CU, D.F., 04510, México e-mail: fdecolle@astroscu.unam.mx

Received: 26 August 2005
Accepted: 17 October 2005

Abstract

Using the Yguazú-a three-dimensional hydrodynamic code, we have computed a set of numerical simulations of heavy, supersonic, radiatively cooling jets including variabilities in both the ejection direction (precession) and the jet velocity (intermittence). In order to investigate the effects of jet rotation on the shape of the line profiles, we also introduce an initial toroidal rotation velocity profile, in agreement with some recent observational evidence found in jets from T Tauri stars which seems to support the presence of a rotation velocity pattern inside the jet beam, near the jet production region. Since the Yguazú-a code includes an atomic/ionic network, we are able to compute the emission coefficients for several emission lines, and we generate line profiles for the Hα, [O I]λ6300, [S II]λ6716 and [N II]λ6548 lines. Using initial parameters that are suitable for the DG Tau microjet, we show that the computed radial velocity shift for the medium-velocity component of the line profile as a function of distance from the jet axis is strikingly similar for rotating and non-rotating jet models. These findings lead us to put forward some caveats on the interpretation of the observed radial velocity distribution from a few outflows from young stellar objects, and we claim that these data should not be directly used as a doubtless confirmation of the magnetocentrifugal wind acceleration models.