000002288 001__ 2288
000002288 005__ 20160706142158.0
000002288 0247_ $$2DOI$$a10.1051/0004-6361/201014562
000002288 037__ $$aASTROimport-445
000002288 100__ $$aDecin, L.
000002288 245__ $$aSilicon in the dust formation zone of IRC +10216
000002288 260__ $$c2010
000002288 520__ $$aThe interstellar medium is enriched primarily by matter ejected from evolved low and intermediate mass stars. The outflows from these stars create a circumstellar envelope in which a rich gas-phase and dust-nucleation chemistry takes place. We observed the nearest carbon-rich evolved star, IRC +10216, using the PACS (55-210 µm) and SPIRE (194-672 µm) spectrometers on board Herschel. We find several tens of lines from SiS and SiO, including lines from the v = 1 vibrational level. For SiS these transitions range up to J = 124-123, corresponding to energies around 6700 K, while the highest detectable transition is J = 90-89 for SiO, which corresponds to an energy around 8400 K. Both species trace the dust formation zone of IRC +10216, and the broad energy ranges involved in their detected transitions permit us to derive the physical properties of the gas and the particular zone in which each species has been formed. This allows us to check the accuracy of chemical thermodynamical equilibrium models and the suggested depletion of SiS and SiO due to accretion onto dust grains. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.Appendix is only available in electronic form at http://www.aanda.org
000002288 700__ $$aCernicharo, J.
000002288 700__ $$aBarlow, M. J.
000002288 700__ $$aRoyer, P.
000002288 700__ $$aVandenbussche, B.
000002288 700__ $$aWesson, R.
000002288 700__ $$aPolehampton, E. T.
000002288 700__ $$aDe Beck, E.
000002288 700__ $$aAgúndez, M.
000002288 700__ $$aBlommaert, J. A. D. L.
000002288 700__ $$aCohen, M.
000002288 700__ $$aDaniel, F.
000002288 700__ $$aDe Meester, W.
000002288 700__ $$aExter, K.
000002288 700__ $$aFeuchtgruber, H.
000002288 700__ $$aFonfría, J. P.
000002288 700__ $$aGear, W. K.
000002288 700__ $$aGoicoechea, J. R.
000002288 700__ $$aGomez, H. L.
000002288 700__ $$aGroenewegen, M. A. T.
000002288 700__ $$aHargrave, P. C.
000002288 700__ $$aHuygen, R.
000002288 700__ $$aImhof, P.
000002288 700__ $$aIvison, R. J.
000002288 700__ $$aJean, C.
000002288 700__ $$aKerschbaum, F.
000002288 700__ $$aLeeks, S. J.
000002288 700__ $$aLim, T.
000002288 700__ $$aMatsuura, M.
000002288 700__ $$aOlofsson, G.
000002288 700__ $$aPosch, T.
000002288 700__ $$aRegibo, S.
000002288 700__ $$aSavini, G.
000002288 700__ $$aSibthorpe, B.
000002288 700__ $$aSwinyard, B. M.
000002288 700__ $$aTercero, B.
000002288 700__ $$aWaelkens, C.
000002288 700__ $$aWitherick, D. K.
000002288 700__ $$aYates, J. A.
000002288 773__ $$cL143$$pAstronomy and Astrophysics$$v518$$y2010
000002288 85642 $$ahttp://esoads.eso.org/abs/2010A%26A...518L.143D
000002288 905__ $$apublished in
000002288 980__ $$aREFERD