Volume 449, Number 3, April III 2006
|Page(s)||1061 - 1066|
|Section||Interstellar and circumstellar matter|
|Published online||24 March 2006|
MHD simulations of radiative jets from young stellar objects
Instituto de Astronomía, Universidad Nacional Autónoma de México, Ap.P. 70264, 04510 DF, Mexico e-mail: email@example.com
2 Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México, Ap.P. 70543, 04510 DF, Mexico
Accepted: 4 October 2005
We study the Hα emission from jets using two-dimensional axisymmetrical simulations. We compare the emission obtained from hydrodynamic (HD) simulations with that obtained from magnetohydrodynamics (MHD) simulations. The magnetic field is supposed to be present in the jet only, and with a toroidal configuration. The simulations have time-dependent ejection velocities and different intensities for the initial magnetic field. The results show an increase in the Hα emission along the jet for the magnetized cases with respect to the HD case. The increase in the emission is due to a better collimation of the jet in the MHD case, and to a small increase in the shock velocity. These results could have important implications for the interpretation of the observations of jets from young stellar objects.
Key words: magnetohydrodynamics (MHD) / shock waves / methods: numerical / Herbig-Haro objects / ISM: jets and outflows / stars: winds, outflows
© ESO, 2006
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