Preprint Logo P75 August
2002


To be published in:
The Astronomical Journal

Structure and dynamics of candidate O star bubbles in N44

Y. Nazé1,*, Y.-H. Chu2,**, M. A. Guerrero2,**, M. S. Oey3, R. A. Gruendl2 and R. Chris Smith4


1 Institut d'Astrophysique et de Géophysique - Université de Liège, Allée du 6 Août, 17, Bât. B5c, B-4000 Liège, Belgium
2 Astronomy Department, University of Illinois, 1002 W. Green Street, Urbana, IL 61801, USA
3 Lowell Observatory, 1400 West Mars Hill Rd., Flagstaff, AZ 86001, USA
4 Cerro Tololo Inter-American Observatory, Casilla 603, La Serena, Chile

* Research Fellow FNRS, Belgium
** Visiting astronomer, Cerro Tololo Inter-American Observatory


Abstract

     Dynamical studies of superbubbles and Wolf-Rayet ring nebulae show discrepancies from the standard, adiabatic model for wind-blown bubbles. We therefore study the physical properties and kinematics of three candidate bubbles blown by single O stars, to evaluate whether these discrepancies are also found in these simpler objects. Our sample candidates are N44F, N44J, and N44M, in the outskirts of the HII complex N44 in the Large Magellanic Cloud. We have obtained ground-based and HST emission-line images and high dispersion echelle spectra for these objects. From the H luminosities and the [OIII]/H ratios of these nebulae, we estimate the spectral types of the ionizing stars to be O7V, O9.5V and O9.5V for N44F, N44J, and N44M, respectively. We find that the observed expansion velocity of 12 km s-1 for N44F is consistent with the stellar wind luminosity expected from the central ionizing star, as predicted by the standard bubble model. The observed upper limits for the expansion velocities of N44J and N44M are also compatible with the expected values, within the uncertainties. We also report the discovery in N44F of strongly-defined dust columns, similar to those seen in the Eagle Nebula. The photoevaporation of these dense dust features may be kinematically important and may actually govern the evolution of the shell. The inclusion of photoevaporation processes may thus undermine the apparent agreement between the observed bubble dynamics and the simple adiabatic models.

Key Words
HII regions -- ISM: bubbles -- ISM: kinematics and dynamics -- ISM: individual (N44) -- Magellanic Clouds

Files
Article: n44.pdf (1948557 bytes): HTTP FTP (ftp://vela.astro.ulg.ac.be/preprints/)


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