Observations of cold dust in S 106

Details Observations of cold dust in S 106 Observations of cold dust in S 106

Aug 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...182..127m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 182, no. 1, Aug. 1987, p. 127-136.

Astronomy and Astrophysics

Astronomy

40

Cosmic Dust, Hydrocyanic Acid, Interstellar Matter, Planetary Nebulae, Stellar Evolution, Angular Resolution, Cross Sections, Radio Sources (Astronomy)

Scientific paper

The authors mapped the bipolar nebula S 106 in the directon of its exciting star IRS 4. They observed cold dust (Td ≡ 18K) emission from a bar-like feature of size 33arcsec× (≤7arcsec) which is approximately centered on IRS 4. Two models can explain the observed characteristics of S 106 and the dust bar. In the geometrical model the dust bar is located behind S 106 and may represent either the cloud core out of which the exciting star IRS 4 of S 106 has formed or it is a dense condensation of cold dust which by chance coincides spatially with S 106. In the physical model, which the authors prefer, the dust bar represents a massive disk surrounding IRS 4 in its equatorial plane. To get agreement with optical and submm dust observations the excitation cross section of dust in visual, i.e. the ratio AV/NH, would have to be decreased by a factor of ≡20 relative to the standard ratio. While formation of mantles of molecular ices can account for some of this, most of the required decrease of AV/NH would probably have to be explained by formation of larger grains due to coagulation.

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