Volume 419, Number 3, June I 2004
|Page(s)||991 - 998|
|Section||Interstellar and circumstellar matter|
|Published online||07 May 2004|
Time-dependent ejection velocity model for the outflow of Hen 3-1475*
Instituto de Ciencias Nucleares, UNAM, Ciudad Universitaria, Apdo. Postal 70-543, CP 04510, Mexico D.F., Mexico e-mail: firstname.lastname@example.org
2 Departament de Física i Enginyeria Nuclear, Universitat Politècnica de Catalunya, Escola Universitària Politècnica de Vilanova i La Geltrú, Av. Víctor Balaguer s/n, 08800 Vilanova i la Geltrú, Spain e-mail: email@example.com
3 Departament d'Astronomia i Meteorologia, Universitat de Barcelona, Av. Diagonal 647, 08028 Barcelona, Spain
Corresponding author: P. F. Velázquez, firstname.lastname@example.org
Accepted: 25 February 2004
We present 2D axisymmetric and 3D numerical simulations of the proto-planetary nebula Hen 3-1475, which is characterized by a remarkably highly collimated optical jet, formed by a string of shock-excited knots along the axis of the nebula. It has recently been suggested that the kinematical and morphological properties of the Hen 3-1475 jet could be the result of an ejection variability of the central source (Riera et al. [CITE]). The observations suggest a periodic variability of the ejection velocity superimposed on a smoothly increasing ejection velocity ramp. From our numerical simulations, we have obtained intensity maps (for different optical emission lines) and position-velocity diagrams, in order to make a direct comparison with the HST observations of this object. Our numerical study allows us to conclude that a model of a precessing jet with a time-dependent ejection velocity, which is propagating into an ISM previously perturbed by an AGB wind, can succesfully explain both the morphological and the kinematical characteristics of this proto-planetary nebula.
Key words: ISM: jets and outflows / planetary nebulae: individual: Hen 3-1475 / methods: numerical / hydrodynamics
© ESO, 2004
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