On the excitation of the infrared knots along protostellar jets

Details On the excitation of the infrared knots along protostellar jets On the excitation of the infrared knots along protostellar jets

2004-02-17

arxiv.org/abs/astro-ph/0402395v1

Astron.Astrophys. 419 (2004) 999-1014

Astronomy and Astrophysics

Astrophysics

15 pages, 15 postscript figures, 3 jpeg figures, accepted by Astronomy and Astrophysics

Scientific paper

10.1051/0004-6361:20040087

The complete near infrared (0.9-2.5 micron) spectra in three different star forming regions (HH24-26, HH72 and BHR71) are presented and analyzed in the framework of shock excitation models. The spectra are dominated by H_2 rovibrational emission (vibrational state nu up to 5, excitation energy T_ex up to 35000 K), while emission from ionized material, recognizable from [Fe II] and [S II] lines, is significantly fainter. The analysis of the H_2 excitation diagrams points to the existence of two different excitation regimes: whilst condensations observed only in the infrared appear to have temperatures rarely exceeding 3000 K and can be modelled in the framework of steady-state C-shock models, the infrared counterparts of Herbig Haro (HH) objects exhibit a temperature stratification with components up to more than 5000 K. The H_2 emission from representative HH objects (HH26A, HH72A and HH320A) has been successfully modelled by planar J-shocks with magnetic precursors, for which the main parameters (pre-shock density, speed) are derived. However, these same models are unable to reproduce the observed atomic and ionic emission, which probably arises from a distinct and perhaps more embedded region with respect to that traced by the H_2. Some of the physical parameters of such regions (fractional ionization, density) have been estimated in HH72, on the basis of the observed ionic lines.

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