Hostname: page-component-78c5997874-mlc7c Total loading time: 0 Render date: 2024-11-16T17:05:37.244Z Has data issue: false hasContentIssue false
  • English
  • Français

Models of Shock Activity in the BN-KL Region of Orion

Published online by Cambridge University Press:  04 August 2017

David Hollenbach ,
C. McKee  and
D. Chernoff
David Hollenbach
Affiliation:
NASA-Ames, CA, USA
C. McKee
Affiliation:
University of California, Berkeley, CA 94720, USA
D. Chernoff
Affiliation:
Cornell University, Ithaca, NY, USA

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The observed H2, CO, OI(63 μm), SiII(34.8 μm) and H51α emission line intensities in the BN-KL region of Orion are modeled as arising from two types of shock waves. The molecular emission arises from non-dissociative shocks with low peak postshock temperatures (< 3000 K), traveling at speeds of vs ∼ 40 km/s into ambient gas of density n0∼105-6 cm−3 and transverse magnetic field B0 ∼0.5 milligauss. The OI(63 μm), Sill(34.8 μm) and H51α emission arises in the cooling regions behind faster (∼80 km/s) dissociative shocks with high peak postshock temperatures (∼105 K) and with preshock densities n0 >3x104 cm−3.

Type
I. Star Forming Processes in the Solar Neighborhood
Information
Symposium - International Astronomical Union , Volume 115: Star Forming Regions , 1987 , pp. 334 - 335
Copyright
Copyright © Reidel 1987