Near-infrared imaging of the jets and flows associated with Herbig-Haro objects HH 91, HH 110, and HH 111

Details Near-infrared imaging of the jets and flows associated with Herbig-Haro objects HH 91, HH 110, and HH 111 Near-infrared imaging of the jets and flows associated with Herbig-Haro objects HH 91, HH 110, and HH 111

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...437l..55d&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 437, no. 1, p. L55-L58

Astronomy and Astrophysics

Astronomy

62

Gas Jets, Herbig-Haro Objects, Infrared Imagery, Kinematics, Shock Waves, Stellar Mass Ejection, Stellar Motions, Emission Spectra, H Alpha Line, Infrared Sources (Astronomy), Limb Brightening, Mixing Layers (Fluids), Turbulent Mixing

Scientific paper

We present near-infrared imaging of the jets and outflows associated with the Herbig-Haro objects HH 91, HH 110 and HH 111. We compare our narrowband H2 nu = 1-0 S(1) (2.121 micron and broadband K images with optical (S II) and H(alpha) images of the same regions. We find that many of the brightest knots in (S II) and H(alpha) have counterparts in H2, although there are some marked differences in morphology. In HH 91 the H2 emission is highly clumpy, like the (S II) emission, although the H2 is mostly confined to the low-excitation regions of the flow. H2 emission also coincides with and outlines the northern edge of a filamentary, optical, 'jetlike' feature in HH 91. We interpret this as possible evidence for entrainment of ambient gas along the northern boundary of this flow. More striking differences between the H2 and optical data are seen in the HH 110 outflow. The 'wiggling' H(alpha) jet appears much straighter in H2. We suggest that close to the source the H2 traces a laminar, mostly molecular jet, while the H(alpha) traces a more extensive turbulent 'mixing layer' that separates the jet from the ambient medium. Also, near HH 110 we have found a second and probably third collimated H2 jet. Neither jet is visible in optical images of the region. Finally, in HH 111 we see the brightest optical features also in H2, including the bow shock at the westerly head of the jet, knot V. Along the jet, the H2 peaks coincide closely with the (S II) knots (after taking into account proper motions), although in knot V the H2 is shifted upstream of the (S II) peak by approximately 1 sec (400 AU): the H2 therefore probably derives from the bow shock wings in knot V.

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