Molecular shock waves in the BN-KL region of Orion

Details Molecular shock waves in the BN-KL region of Orion Molecular shock waves in the BN-KL region of Orion

Aug 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...259l..97c&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor, vol. 259, Aug. 15, 1982, p. L97-L101.

Astronomy and Astrophysics

Astrophysics

169

Interstellar Gas, Magnetohydrodynamic Waves, Molecular Gases, Orion Nebula, Shock Waves, Astronomical Models, Carbon Monoxide, Hydrogen, Hydroxyl Radicals, Infrared Spectra, Interstellar Magnetic Fields

Scientific paper

The H2, CO, and OH IR emission-line intensities in the BN-KL region of Orion are modeled by shock waves traveling at 36 km/s with respect to an ambient gas of density 200,000 per cu cm, ionization fraction of less than 3 x 10 to the -7th, CO abundance of approximately 0.0003, and transverse magnetic field of 0.45 milligauss. A global model is considered in which the shock waves are driven by strong winds emanating from KL. The mass-loss rate has been not less than 0.003 solar mass per year for approximately 1000 years. The total wind energy released from the star is not less than 5 x 10 to the 47th ergs. The total ejected momentum is approximately 10 to the 41st g cm/S, sufficient to disrupt the dense cloud surrounding BN-KL.

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