Molecular shock waves in the BN-KL region of Orion

Journal Article · Sun Aug 15 04:00:00 EDT 1982 · Astrophys. J., Lett. Ed.; (United States)

DOI:https://doi.org/10.1086/183855· OSTI ID:7041006

Chernoff, D F; Hollenbach, D J; McKee, C F

The H/sub 2/, CO, and OH infrared emission-line intensities in the BN-KL region of Orion are modeled by shock waves traveling at v/sub S/roughly-equal36 km s/sup -1/ with respect to ambient gas of density n/sub O/roughly-equal2 x 10/sup 5/ cm/sup -3/, ionization fraction x/sub i/0<3 x 10/sup -7/, CO abundance of approximately 3 x 10/sup -4/, and transverse magnetic field B/sub 0perpendicular/0.45 milligauss. The inferred preshock magnetic energy density may help support the cloud. The extinction to the 2 ..mu..m H/sub 2/ emission is approximately 2--2.5 mag. The high-velocity wings of the H/sub 2/ emission lines are produced by slow nondissociative shocks incident upon high-speed ambient gas or behind fast dissociative shocks. A global model is described in which the shock waves are driven by strong winds emanating from KL. The mass-loss rate has been > or approx. =3 x 10/sup -3/ M/sub sun/ yr/sup -1/ for a time of approximately 10/sup 3/ years. The total wind energy released from the star is E> or approx. =5 x 10/sup 47/ ergs. The total ejected momentum is about 10/sup 41/ g cm s/sup -1/, sufficient to disrupt the dense cloud surrounding BN-KL.

• Research Organization: University of California, Berkeley
• OSTI ID: 7041006
• Journal Information: Astrophys. J., Lett. Ed.; (United States), Journal Name: Astrophys. J., Lett. Ed.; (United States) Vol. 259:2; ISSN AJLEA
• Country of Publication: United States
• Language: English

Related Subjects

640105* -- Astrophysics &amp; Cosmology-- Galaxies
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
CARBON COMPOUNDS
CARBON MONOXIDE
CARBON OXIDES
CHALCOGENIDES
COSMIC GASES
ELEMENTS
EMISSION SPECTRA
FLUIDS
GASES
HYDROGEN
HYDROGEN COMPOUNDS
HYDROMAGNETIC WAVES
HYDROXIDES
INFRARED SPECTRA
INTERSTELLAR GRAINS
NEBULAE
NONMETALS
OXIDES
OXYGEN COMPOUNDS
PARTICLES
SHOCK WAVES
SPECTRA
STELLAR WINDS