Galactic environment and the 10-μm silicate feature of young stellar objects

Details Galactic environment and the 10-μm silicate feature of young stellar objects Galactic environment and the 10-μm silicate feature of young stellar objects

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003mnras.340.1173b&link_type=abstract

Monthly Notice of the Royal Astronomical Society, Volume 340, Issue 4, pp. 1173-1189.

Astronomy and Astrophysics

Astronomy

11

Circumstellar Matter, Infrared: Stars

Scientific paper

Disc and sphere dust models are used to fit 8-13 μm flux spectra of 19 low-mass young stellar objects (YSOs) and five Herbig AeBe stars. The 13 non-photospheric low-mass YSOs in quiescent environments and the five Herbig AeBe stars have mean disc temperature indices of 0.4, indicating that the emission arises from optically thin layers above a flared optically thick disc; 10 out of 14 of the low-mass YSO and four out of five of the Herbig AeBe features contain an optically thin silicate emission component. The radius of the peak 10-μm emission for nine out of the 13 low-mass YSOs is 10-130 au, and three out of the five Herbig AeBe stars are 10-30 au in size. In contrast, the five YSOs from disrupted molecular clouds that have been shaped by expanding supernova remnants have temperature indices of between 0.3 and 0.8; four out of the five are optically thick and three out of the five have radii <~2 au. The photosphere-like continuum of Taurus-Elias 18 could be fitted only with truncated optically thick models, implying the presence of a void between the >500 K and cold (<~100 K) foreground dust. Silicates surrounding low-mass YSOs in quiescent molecular clouds are similar to those in the Trapezium region of the Orion Nebula except when AV<~ 2 mag. In the low-AV case and in low-mass YSOs in disrupted molecular clouds the silicates are similar to circumstellar dust around the evolved star μ Cephei.

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