Mid-infrared interferometry on spectral lines: III. Ammonia and Silane around IRC+10216 and VY CMa

Details Mid-infrared interferometry on spectral lines: III. Ammonia and Silane around IRC+10216 and VY CMa Mid-infrared interferometry on spectral lines: III. Ammonia and Silane around IRC+10216 and VY CMa

2000-07-27

arxiv.org/abs/astro-ph/0007418v1

Astronomy and Astrophysics

Astrophysics

31 Pages, Accepted in the Astrophysical Journal

Scientific paper

10.1086/317127

Using the U.C. Berkeley Infrared Spatial Interferometer with an RF filterbank, the first interferometric observations of mid-infrared molecular absorption features of ammonia (NH_3) and silane (SiH_4) with very high spectral resolution (R ~ 100000) were made. Under the assumptions of spherical symmetry and uniform outflow, these new data permitted the molecular stratification around carbon star IRC+10216 and red supergiant VY CMa to be investigated. For IRC+10216, both ammonia and silane were found to form in the dusty outflow significantly beyond both the dust formation and gas acceleration zones. Specifically, ammonia was found to form before silane in a region of decaying gas turbulence (>~ 20 R_star), while the silane is produced in a region of relatively smooth gas flow much further from the star (>~ 80 R_star). The depletion of gas-phase SiS onto grains soon after dust formation may fuel silane-producing reactions on the grain surfaces. For VY CMa, a combination of interferometric and spectral observations suggest that NH_3 is forming near the termination of the gas acceleration phase in a region of high gas turbulence (~ 40 R_star).

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