Cometary compact H II regions are stellar-wind bow shocks

Details Cometary compact H II regions are stellar-wind bow shocks Cometary compact H II regions are stellar-wind bow shocks

Apr 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...353..570v&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 353, April 20, 1990, p. 570-578. Research supported by the Alan and Dorothy

Astronomy and Astrophysics

Astrophysics

148

Bow Waves, H Ii Regions, Shock Wave Propagation, Stellar Winds, Astronomical Models, Comets, Interstellar Masers, Nebulae

Scientific paper

Comet-shaped H II regions, like G34.3 + 0.2, are easily explained as bow shocks created by wind-blowing massive stars moving supersonically through molecular clouds. The required velocities of the stars through dense clumps are less than about 10 km/s, comparable to the velocity dispersion of stars in OB associations. An analytic model of bow shocks matches the gross characteristics seen in the radio continuum and the velocity structure inferred from hydrogen recombination and molecular line observations. The champagne flow model cannot account for these structures. VLBI observations of masers associated with the shells of cometary compact H II regions should reveal tailward proper motions predominantly parallel to the shell, rather than perpendicular. It is predicted that over a decade baseline, high signal-to-noise VLA observations of this class of objects will show headward pattern motion in the direction of the symmetry axis, but not expansion. Finally, shock-generated and coronal infrared lines are also predicted.

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