High resolution simulations of a variable HH jet

¹ Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México, Ap. 70-543, 04510, DF México e-mail: [raga;esquivel]@nucleares.unam.mx
² Dublin Institute of Advanced Studies, 5 Merrion Sq., Dublin, Ireland e-mail: fdc@cp.dias.ie
³ Instituto de Astronomía, Universidad Nacional Autónoma de México, Ap. 70-264, 04510, DF México e-mail: primoz@astroscu.unam.mx

Received: 24 October 2006
Accepted: 30 December 2006

Abstract

Context.In many papers, the flows in Herbig-Haro (HH) jets have been modeled as collimated outflows with a time-dependent ejection. In particular, a supersonic variability of the ejection velocity leads to the production of “internal working surfaces” which (for appropriate forms of the time-variability) can produce emitting knots that resemble the chains of knots observed along HH jets.

Aims.In this paper, we present axisymmetric simulations of an “internal working surface” in a radiative jet (produced by an ejection velocity variability). We concentrate on a given parameter set (i.e., on a jet with a constante ejection density, and a sinusoidal velocity variability with a 20 yr period and a 40 km s^-1 half-amplitude), and carry out a study of the behaviour of the solution for increasing numerical resolutions.

Methods.In our simulations, we solve the gasdynamic equations together with a 17-species atomic/ionic network, and we are therefore able to compute emission coefficients for different emission lines.

Results.We compute 3 adaptive grid simulations, with 20, 163 and 1310 grid points (at the highest grid resolution) across the initial jet radius. From these simulations we see that successively more complex structures are obtained for increasing numerical resolutions. Such an effect is seen in the stratifications of the flow variables as well as in the predicted emission line intensity maps.

Conclusions.We find that while the detailed structure of an internal working surface depends on resolution, the predicted emission line luminosities (integrated over the volume of the working surface) are surprisingly stable. This is definitely good news for the future computation of predictions from radiative jet models for carrying out comparisons with observations of HH objects.