2012
DOI: 10.1051/0004-6361/201218953
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Non-local radiative transfer of SiO masers in Miras

Abstract: Context. To properly understand the propagation of SiO masers within the shocked region of the circumstellar envelope of asymptotic giant branch stars, non-local radiative transfer calculations are required. Aims. The present study focuses on investigating how the non-linear velocity field affects the amplification of SiO masers in the circumstellar envelope of a Mira variable. Methods. We extend the capability of the coupled escape probability method to a spherical system and develop subroutines that are able… Show more

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Cited by 11 publications
(5 citation statements)
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References 57 publications
(111 reference statements)
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“…We have counted a total of 33 sources (44%) where F(v = 2) is greater than F(v = 1), and 42 cases (56%) with the opposite behavior. Overall results of this rather simple analysis seem to confirm the prediction made by Yun & Park (2012), although a more thorough and case-bycase analysis should be performed to provide a firm confirmation.…”
Section: About the Emitting Regionsupporting
confidence: 62%
“…We have counted a total of 33 sources (44%) where F(v = 2) is greater than F(v = 1), and 42 cases (56%) with the opposite behavior. Overall results of this rather simple analysis seem to confirm the prediction made by Yun & Park (2012), although a more thorough and case-bycase analysis should be performed to provide a firm confirmation.…”
Section: About the Emitting Regionsupporting
confidence: 62%
“…On the other hand, the non-local radiative transfer (RT) model occasionally shows a slightly wider velocity range of the 86.2 GHz maser than the 43.1 GHz maser, supporting our observational results (Yun & Park 2012;McIntosh & Indermuehle 2015).…”
Section: Resultssupporting
confidence: 88%
“…However, the non-local RT model has never predicted that the 86.2 GHz maser features could appear at a smaller radius than those of the 43.1 GHz maser. The non-local RT model (Yun & Park 2012) used the hydrodynamic solutions for a fundamental-pulsator. Therefore, further studies of the non-local RT model based on the hydrodynamic CSE model for overtone-pulsators are required for interpreting our results and for evaluating the effect of different pulsation modes on the various SiO maser features.…”
Section: Comparison Among Thementioning
confidence: 99%
“…Even if a particular maser feature represents the local velocity, the single-dish results can represent the velocity dispersion of the entire velocity field because it detects all of the combined velocity components without exception. The emitting regions of SiO masers are accelerated, and the acceleration decreases as distance increases, although the motion inside the dust layer is complicated (Yun & Park 2012). The velocity dispersion of the maser lines of the 42.8 GHz SiO maser could be smaller than that of other SiO masers, since it is located in the large velocity gradient region close to the central star, which could yield a small FWZP.…”
Section: Full Width At Zero Power Variations Of H 2 O and Sio Masersmentioning
confidence: 99%