IRAS low resolution spectrograph spectral class and M and S Miras

Details IRAS low resolution spectrograph spectral class and M and S Miras IRAS low resolution spectrograph spectral class and M and S Miras

Jan 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...209..165v&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 209, no. 1-2, Jan. 1989, p. 165-172.

Astronomy and Astrophysics

Astronomy

9

Light Curve, M Stars, Mira Variables, S Stars, Stellar Spectra, Absorption Spectra, Emission Spectra, Infrared Astronomy Satellite, Silicates, Stellar Envelopes

Scientific paper

A large sample of 177 M and S Miras, as revealed by their IRAS LRS spectral class, have been examined to determine the dependence of silicate emission on the visual light curve asymmetry factor, f. It is confirmed that 9.7-micron silicate emission feature not only in M but in S Miras also occurs only when f is not greater than 0.45. However, not all stars with f of not greater than 0.45 show the silicate emission; this nondetection reveals dependence on other parameters like the mean visual light amplitude. Though strong emission feature in M Miras may occur for any value of f, very weak features are absent for small values of f, and the strongest features tend to appear for larger values of f. Infrared excess tends to increase with the strength of the silicate emission as well as with decrease in the value of f. The probability of detection of silicate emission is very high for the visual light curve classes (Ludendorff, 1928) alpha 1, alpha 2, and alpha 3, decreases for alpha 4 and gamma 1, and is negligible for the beta class.

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