Other
Scientific paper
Dec 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.1606p&link_type=abstract
American Astronomical Society, 181st AAS Meeting, #16.06; Bulletin of the American Astronomical Society, Vol. 24, p.1147
Other
Scientific paper
The (29) SiO (2-1) transition at 85.76 GHz and the HC(15) N (1-0) transition at 86.05 GHz have been detected in absorption towards the middle and northern HII region complexes in Sgr B2 with the BIMA array at a resolution of 7.9times 4.6". The (29) SiO line is significantly narrower than the HC(15) N line and most other molecular absorption lines, which suggests that shocks do not produce the observed SiO enhancement, unlike in many other sources. The velocity and line width of the (29) SiO absorption line most closely resemble the NH_3 (8,8) and (9,9) absorption lines observed by Wilson et al. (1982), which implies that the SiO absorption arises in the same extended hot (175 K), low density (10(4) cm(-3) ) gas as the hot NH_3. We suggest that the SiO enhancement in the gas seen in absorption is due to evaporation of grain mantles at the high observed temperatures, which releases a fraction of the Si into the gas phase. The SiO abundance in the extended low density gas is much larger than derived by Sutton et al. (1991) for the compact Sgr B2 outflows, which have enhancements that are small compared to local outflows. The low enhancements in the Sgr B2 outflows can be attributed to their relatively high densities, which lead to short timescales for depletion of the SiO on to dust grains.
Peng Yuan
Vogel Stuart
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