The spectral energy distribution of star-forming regions

Details The spectral energy distribution of star-forming regions The spectral energy distribution of star-forming regions

May 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...408..218s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 408, no. 1, p. 218-229.

Astronomy and Astrophysics

Astronomy

26

Astronomical Models, Cosmic Dust, Spectral Energy Distribution, Star Formation, Stellar Envelopes, Infrared Astronomy, Interstellar Extinction, Radiative Transfer

Scientific paper

We present exact solutions of the radiative transfer problem for clouds containing quantum-heated dust particles, with attention to dust destruction as appropriate for modeling star-forming regions. The dust model by Siebenmorgen and Kruegel (1993) is compared with models containing only large grains heated under steady state conditions. We demonstrate that both models can be distinguished by studying the surface brightness morphology of objects at midinfrared wavelengths. The emission bands of polycyclic aromatic hydrocarbons in media with high optical depth is studied and the multicomponent grain emission and temperature structures inside opaque clouds is discussed. We present excellent fits of a sample of well-known star-forming regions by calculating beam-matched spectral energy distributions. The current problems of modeling the infrared emission from star-forming regions are summarized. We suggest that a scenario of disklike structures embedded in the circumstellar dust envelope might better match the observations. The disk grains should be large and of inhomogeneous structure. The grain absorption cross sections of fluffy grains are calculated by using the Maxwell-Garnett mixing rule. We find that compositional inhomogeneities of dust grains will affect the silicate bands and increase the absorptivity at far-infrared and submillimeter wavelengths.

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