An Improved Model of SiO Maser Emission in Miras

Details An Improved Model of SiO Maser Emission in Miras An Improved Model of SiO Maser Emission in Miras

2008-11-17

arxiv.org/abs/0811.2770v1

2009MNRAS.394...51G

Astronomy and Astrophysics

Astrophysics

accepted by MNRAS, MN-08-1478-MJ.R1

Scientific paper

10.1111/j.1365-2966.2008.14237.x

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 infra-red (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 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 to 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\micron appear to be closely associated in three out of four phase samples.

Affiliated with

Also associated with

No associations

Rating

An Improved Model of SiO Maser Emission in Miras does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with An Improved Model of SiO Maser Emission in Miras, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and An Improved Model of SiO Maser Emission in Miras will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-467322