Physics – Plasma Physics
Scientific paper
Jan 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21336004p&link_type=abstract
American Astronomical Society, AAS Meeting #213, #360.04; Bulletin of the American Astronomical Society, Vol. 41, p.510
Physics
Plasma Physics
1
Scientific paper
Newly formed hot stars clearly interact with and shape the surrounding molecular gas from which they form, but there are several possible feedback processes: supernovae, stellar winds, thermal gas pressure and/or radiation pressure. Our aim is to calibrate the important physical processes of larger star forming regions at distances too great to be spatially resolved using the Orion nebula with one O star, M17 with about 10, up to NGC 3603 and 30 Doradus with up to 100 O stars. Here we present a new survey of optical spectra over much of NGC 3603 and 30 Doradus covering the Hα, Hβ, [O III] and [S II] emission lines. A subsample of positions was also observed with long-slit K-Band spectroscopy. In addition to the spectra, we have obtained high resolution, narrow-band images of NGC 3603 and 30 Doradus covering 8'x10’ and 12'x13’ respectively, in Hα, [SII] and [OIII] plus continuum passbands. These fill in the gaps between the spectra. These images are up to 10 times higher resolution than the Magellanic Cloud Emission Line Survey and cover a field of view 12 times larger than HST.
By combining X-ray, optical, IR and radio observations we constrain our self-consistent models through the H+ , H0 and molecular regions, allowing us to study the physical nature of the interaction of stars and their parent molecular cloud. The optical spectra fill in gaps to the available data set including a large scale mapping of the electron density measured from the [SII] emission which is a critical constraint in the construction of simulated lines of sight using the plasma physics code CLOUDY. The measurements together with the models allow us to compare the relative importance of gas pressure, radiation pressure, stellar winds and the hot X-ray emitting component resulting from massive star formation.
Baldwin John A.
Ferland Gary J.
Pellegrini Eric W.
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