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The infrared emission from dust surrounding newly formed O stars
Churchwell, E.; Wolfire, M. G.; Wood, Douglas O. S.
AA(Wisconsin, University, Madison), AB(Chicago, University, IL), AC(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 354, May 1, 1990, p. 247-261. (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Cosmic Dust, Emission Spectra, Infrared Radiation, O Stars, Star Formation, Absorption Spectra, Abundance, Density Distribution, Ionized Gases, Molecular Clouds, Radiative Transfer, Stellar Envelopes
Bibliographic Code:


The dust cocoon around a newly formed 06 ZAMS star embedded in its natal molecular cloud is modeled for a wide range of radial density distribution and grain properties. The most important result of this investigation is that the only models that satisfy all the observational constraints require thin dust shells with relatively large inner radii composed of grains with about one-half the graphite/silicate abundance ratio of the MRN-DL mixture for the diffuse interstellar medium. It is also shown that constant density models produce the best overall fit to the observations; the dust cocoons are optically thick at wavelengths shortward of approximately 7 microns, and the warm dust cocoons are large; the average dust temperatures drop very steeply just outside the inner boundary of the dust shell to less than 100 K in less than 0.1 percent of the outer shell radius; the addition of water ice mantles to refractory grain cores produces a strong 3.07 micron absorption feature and weaker 12 and 45 micron absorption features; and all models imply rather massive dust shells.

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