The excitation of molecular hydrogen in HH 1 and in HH 7 to 11.

Details The excitation of molecular hydrogen in HH 1 and in HH 7 to 11. The excitation of molecular hydrogen in HH 1 and in HH 7 to 11.

Jan 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...305..582g&link_type=abstract

Astronomy and Astrophysics, v.305, p.582

Astronomy and Astrophysics

Astrophysics

43

Ism: Clouds, Ism: Jets And Outflows, Ism: Molecules, Infrared: Interstellar: Lines And Bands, Stars: Pre Main-Sequence

Scientific paper

Results are presented on spectroscopic observations of near-infrared molecular hydrogen emission lines towards the Herbig-Haro objects HH 1 and HH 7 to 11. The inferred population densities in the observed H_2_ levels towards HH 1 and HH 11 are well described by pure thermal distributions, and single excitation temperatures provide good fits. None of the levels have a significantly enhanced population density as should occur if non-thermal processes were involved. The H_2_ emission towards HH 1 arises from collisional excitations in a gas of temperature around 2750K, while contributions from FUV pumping, suggested elsewhere, are not present. The emission from HH 11 arises from gas at similar temperatures, and emission from H_2_ re-formation is ruled out. Near-infrared emission of [FeII], present towards HH 1 and HH 7 to 11, is used to infer a reddening of E_B-V_=~0.5mag and an electron density of n_e_=~5000cm^-3^ towards HH 1. Towards individual knots in HH 7 to 11, reddenings range from E_B-V_=2 to 7mag. The H_2_ and [FeII] observations together suggest the presence of curved J-type shocks, and rule out C-type bow shocks as the origin of the emission.

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