VLA recombination line observations of the cometary H II region G34.3+0.2: Dynamics and physical properties

Details VLA recombination line observations of the cometary H II region G34.3+0.2: Dynamics and physical properties VLA recombination line observations of the cometary H II region G34.3+0.2: Dynamics and physical properties

Sep 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...432..648g&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 432, no. 2, p. 648-655

Other

52

Astronomical Models, Bow Waves, Emission Spectra, H Alpha Line, H Ii Regions, Shock Waves, Stellar Winds, Velocity Distribution, Interstellar Masers, Ionized Gases, Molecular Clouds, Radio Emission, Star Formation, Very Large Array (Vla)

Scientific paper

We have observed the H93(alpha) radio recombination line emission toward the cometary H II region G34.3+0.2 component C. A velocity gradient with a total extent of approximately equal 35 km/s is found in the H93(alpha) line emission perpendicular to the symmetry axis of the cometary H II region. A smaller velocity gradient is found parallel to the symmetry axis. The moving star bow shock model and the champagne outflow model have been suggested to explain observations of G34.3+0.2C. Neither model adequately matches the available velocity data. G34.3+0.2 components A and B are found near G34.3+0.2C. The continuum spectral indices of components A and B are consistent with that expected for an ionized wind outflow. We suggest a qualitative model for the region where the ionizing star of the cometary H II region G34.3+0.2C photo-evaporates material from a hot ultracompact molecular core found just to the east of the continuum emission. Interaction between the ionized gas of the cometary H II region and winds from components A and B may explain many of the current observations. We have also mapped the 616 goes to 523 transition of H2O toward G34.3+0.2. We find strong H2O maser emission within a approximately equals 50 sec x 30 sec region. Some of the H2O masers are projected onto sources of radio continuum emission, but others are found well separated from radio continuum emission.

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