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Molecular hydrogen jets from the Orion nebula

Nature volume 311, pages 236–237 (1984)Cite this article

Abstract

The environs of interstellar space in which star formation takes place involve high-velocity gas flows. Channelled by embryonic dust toroids, these gas flows culminate in energy-losing shock processes at the interface with the ambient interstellar cloud. The excitation of molecular hydrogen transitions in this gas provides one means of observing these shocked regions and their relation to the well-known indicators of star formation such as the Herbig Haro objects and T Tauri stars. In an attempt to understand the relationship of the recently discovered complex of Herbig Haro objects in Orion1 to the IR sources in this region, we have carried out a survey of the molecular hydrogen S(1) line distribution. These observations have led to the discovery of a previously unsuspected structure of finger-like filaments of H2 emission extending radially outwards from a common centre at IRC9.

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Authors and Affiliations

  1. Optical Science and Technology, University of New South Wales, Kensington, 2033, Australia

    K. N. R. Taylor & J. W. V. Storey

  2. Astrophysics Laboratory, University of Helsinki, Helsinki, 13, Finland

    G. Sandell

  3. United Kingdom Infrared Telescope Unit, 900 Leilani Street, Hilo, Hawaii, 96720, USA

    P. M. Williams

  4. Royal Observatory, Blackford Hill, Edinburgh, EH9 3HJ, UK

    W. J. Zealey

Authors
  1. K. N. R. Taylor
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  2. J. W. V. Storey
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  3. G. Sandell
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  4. P. M. Williams
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  5. W. J. Zealey
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Taylor, K., Storey, J., Sandell, G. et al. Molecular hydrogen jets from the Orion nebula. Nature 311, 236–237 (1984). https://doi.org/10.1038/311236a0

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