Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...442..674s&link_type=abstract
Astrophysical Journal (ISSN 0004-637X), vol. 442, no. 2, Part 1, p. 674-678
Astronomy and Astrophysics
Astronomy
10
Gas Jets, Hydrogen, Infrared Astronomy, Interstellar Matter, Molecular Clouds, Molecular Flow, Molecular Gases, Molecular Spectra, Orion Nebula, Astronomical Spectroscopy, Data Reduction, Red Shift, Spatial Distribution, Spectrum Analysis, Velocity Distribution
Scientific paper
The velocity field of the H2 nu = 1-0 S(1) line in the orion-KL region was measured using a Fabry-Perot imager with 24 km/s resolution. The peak velocity is bluest near the central source, approaching the rest velocity of the ambient molecular cloud with increasing distance from the center. This spatial variation of the peak velocity can be explained by an expanding spherical shell. The radius of the shell is coincident with the extent of the high-velocity molecular outflow, which drives the shell expansion. Blue wings, which reflect the motion of shocked gas in the outflow, show also an approximately spherical expansion. These results imply a more or less originally isotropic flow from the central source. A curved, bridgelike structure that encroaches on the inner edge of a disk structure is noticeable in the peak velocity map, with the bluest peak velocities. This structure is considered to be a region where the isotropic outflow from the central source strongly collides with the inner edge of the disk, which imposes a bipolar appearance on the flow.
Inoue Motoko Y.
Kataza Hirokazu
Kawabata Hironobu
Sugai Hajime
Tanaka Masuo
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