A model for the intense molecular line emission from OMC-1

A model for the intense molecular line emission from OMC-1

We present a model which attributes the observed H/sub 2/ and CO line emission OMC-1 to a magnetohydrodynamic shock propagating into magnetized molecular gas. By requiring the shock to reporoduce the observed line intensities, we determine the shock speed to be v/sub s/roughly-equal38 km s/sup -1/ a...

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Veröffentlicht in:Astrophys. J., Lett. Ed.; (United States) Lett. Ed.; (United States), 1982-08, Vol.259, p.L91
Hauptverfasser: Draine, B. T., Roberge, W. G.
Format: Artikel
Sprache:eng
Schlagworte:
CARBON COMPOUNDS
CARBON MONOXIDE
CARBON OXIDES
CHALCOGENIDES
CHEMISTRY
CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS
COSMIC GASES
COSMOCHEMISTRY
ELEMENTS
EMISSION SPECTRA
ENERGY LEVELS
ENERGY-LEVEL TRANSITIONS
EXCITED STATES
FLUIDS
GASES
HYDROGEN
HYDROMAGNETIC WAVES
INFRARED SPECTRA
INTERSTELLAR MAGNETIC FIELDS
MAGNETIC FIELDS
MOLECULES
NEBULAE
NONMETALS
OXIDES
OXYGEN COMPOUNDS
ROTATIONAL STATES
SHOCK WAVES
SPECTRA 640105 > Astrophysics & Cosmology-- Galaxies
WAVE PROPAGATION
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Zusammenfassung:We present a model which attributes the observed H/sub 2/ and CO line emission OMC-1 to a magnetohydrodynamic shock propagating into magnetized molecular gas. By requiring the shock to reporoduce the observed line intensities, we determine the shock speed to be v/sub s/roughly-equal38 km s/sup -1/ and the preshock density and (transverse) magnetic field to be n/sub H/roughly-equal7 x 10/sup 5/ cm/sup -3/, B/sub O/roughly-equal1.5 milligauss. The model is compared to observations of H/sub 2/, CO, OH, O I, and C I in emission and of CO in absorption. The shock gas may be detectible in H I 21 cm emission.
ISSN:0004-637X
1538-4357
DOI:10.1086/183854