The Near Circumstellar Environment of Miras

Details The Near Circumstellar Environment of Miras The Near Circumstellar Environment of Miras

Jul 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985mlrg.proc...85h&link_type=abstract

Mass Loss from Red Giants; Proceedings of the Conference, University of California, Los Angeles, CA, June 20, 21, 1984. Edited

Astronomy and Astrophysics

Astrophysics

1

Scientific paper

Time series spectra were used to analyze the CO Δv = 2 spectrum (2.3 - 2.5 μm) of 5 Miras and 1 SRa variable. A similar analysis previously was undertaken for the S-type Mira χ Cyg (Hinkle, Hall and Ridgway 1982). The Δv = 2 spectrum of long period variables is complex with high excitation lines originating entirely in the (IR) photosphere and the lower excitation lines being formed through the photosphere and one or two extended atmospheric regions. The photospheric lines are characterized by large amplitude velocity and temperature changes with a mean excitation temperature of ≡3000K (Hinkle, Scharlach and Hall 1984). In contrast, the extended atmospheric regions exhibit much smaller velocity changes plus lower and near stable excitation temperature.

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