{"references": ["Benson, P. J. & Little-Marenin, I. R. 1996, ApJS, 106, 579", "Bergeat, J., Sibille, F., Lunel, M., & Lefevre, J. 1976, A&A, 52, 227", "Bidelman, W. P. 1954, ApJS, 1, 175", "Creech-Eakman, M. J., G\u00fcth, T., Luttermoser, D. G., Jurgen- son, C. A., & Speck, A. K. 2012, The Astronomical Review, 7, 4", "Duner, N. C. 1899, ApJ, 9", "Feuchter, A. C. 1967, AJ, 72, 702", "Houck, J. R., Roellig, T. L., Van Cleve, J., Forrest, W. J., Herter, T. L., et al. 2004, In Optical, Infrared, and Millimeter Space Telescopes, edited by J. C. Mather, Proceedings of the Spie, vol. 5487, pp. 62\u201376", "Luttermoser, D. G. & Mahar, S. 1998, In Cool Stars, Stellar Sys- tems, and the Sun, edited by R. A. Donahue & J. A. Book- binder, Astronomical Society of the Pacific Conference Se- ries, vol. 154, p. 1613", "Pickering, E. C. & Fleming, W. P. 1905, ApJ, 22", "Sivagnanam, P., Le Squeren, A. M., & Foy, F. 1988, A&A, 206, 285", "van Belle, G. T., Dyck, H. M., Thompson, R. R., Benson, J. A., & Kannappan, S. J. 1997, AJ, 114, 2150", "Willson, L. A. 1972, A&A, 17, 354"]}

We present preliminary analysis of mid-infrared spectra of M-type and C-type Mira variables. Due to the brightness of this sample, it is straightforward to monitor changes with phase in the infrared spectral features of these regular pulsators. We have spectra of 25 Mira variables, taken with phase, using the Spitzer Infrared Spectrograph (IRS) high-resolution module. Each star has multiple spectra obtained over a one-year period from 2008-09. This is a rich, unique data set due to multiple observations of each star and the high signal-to-noise ratio from quick exposure times to prevent saturation of the IRS instrument. This paper focuses on the 17.6 and 33.2 micron lines shared by M-types and C-types. These are mostly emission lines that change with phase. We discuss preliminary physical diagnostics for the atmospheres based on the lines, as well as possible line identifications such as fluorescence of metal species.

Poster #171