Abstract
The cool molecular region of late-type stellar atmospheres, the ‘MOLsphere’ located between the photosphere and expanding circumstellar shell, is explored by using time series of near-IR spectra of one large amplitude AGB (Mira) variable. The ∼⃒1400 K MOLsphere of the Mira R Cas is shown to undergo large amplitude velocity changes that are aperiodic with time scales many times longer than the photospheric pulsation. The mass of the MOLsphere is ∼⃒3×10−5 M⊙. Initial analysis suggests that MOLsphere is thin compared to the stellar radius.
Highlights
For low mass stars the majority of the mass loss occurs during the AGB evolutionary phase
The atmospheric carbon and oxygen isotopic ratios are altered by the CNO cycle, He burning, and mixing processes that take place in the stellar interior over the lifetime of the star [12]
By measuring carbon and oxygen isotopic ratios we demonstrate that most unobscured Miras in the solar neighborhood had progenitor masses ≤ 2 M [11]
Summary
This content has been downloaded from IOPscience. Please scroll down to see the full text. Ser. 728 022003 (http://iopscience.iop.org/1742-6596/728/2/022003) View the table of contents for this issue, or go to the journal homepage for more. Download details: IP Address: 131.130.87.199 This content was downloaded on 01/06/2017 at 10:45 Please note that terms and conditions apply
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Free) 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
