2008/11/17 by M. D. Gray, M. Wittkowski, M. Scholz +4
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Galaxies: Formation, Evolution, Phenomena #Infrared #Maser #Optics #Photosphere #Physics #RADIUS #Shock wave #Spectral line #Stellar, planetary, and galactic studies #Very-long-baseline interferometry #Wavelength #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2008.14237.x
published as 2009MNRAS.394...51G · accepted by MNRAS, MN-08-1478-MJ.R1
arxiv created 2008/11/17 · openalex publication_date 2009/02/20 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We describe a combined dynamic atmosphere and maser propagation model of SiO maser emission in Mira variables. This model rectifies many of the defects of an earlier model of this type, particularly in relation to the infrared (IR) radiation field generated by dust and various wavelength-dependent, optically thick layers. Modelled masers form in rings with radii consistent with those found in very long baseline interferometry (VLBI) observations and with earlier models. This agreement requires the adoption of a radio photosphere of radius approximately twice that of the stellar photosphere, in agreement with observations. A radio photosphere of this size renders invisible certain maser sites with high amplification at low radii, and conceals high-velocity shocks, which are absent in radio continuum observations. The SiO masers are brightest at an optical phase of 0.1–0.25, which is consistent with observed phase lags. Dust can have both mild and profound effects on the maser emission. Maser rings, a shock and the optically thick layer in the SiO pumping band at 8.13 μm appear to be closely associated in three out of four phase samples.