Titlebook: Cool Stars with Excesses of Heavy Elements; Proceedings of the S Mercedes Jaschek,Philip C. Keenan Conference proceedings 1985 D. Reidel Pu

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Reliability Improvement Warranties,he atmospheric structure of carbon stars: Because of the increased line-blanketing(backwarming) effect due to increased molecular absorption in cooler stars, kinetic temperature of the line formation layers shows little decrease for large decrease of the effective temperature (e.g., △T.(FeI)=250K fo

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Systems Approach to Warranty Management, CN and CH anomalies, metal deficiencies and interstellar reddening. It also turns out to be a very powerful tool for monitoring the variability of the cool stars. The identification of the observed spectra and the computation of the partial pressure versus optical depth via model atmospheres demons

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Identification of Photographic Infrared Spectral Region in Carbon Starsconnection with the identification of .CN, .CN, HCN, [CI] λ8727, and telluric H.O lines. The microphotometric tracing of the same region of an M-type star μ Cep seems very helpful for the identification of telluric H.O lines.

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The Discovery and Frequency of Barium Starsristics of H.D. barium-star suspects south of δ = -26? found on moderate-dispersion objective-prism plates. For stars of the type that can be found from such plates, the frequency appears to lie between one-half and one percent.

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Astrophysics and Space Science Libraryhttp://image.papertrans.cn/c/image/237886.jpg

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Prevention of Controller Windup,Some correlations between period of pulsation, spectral type at maximum, mean difference in visual magnitude between maxima and minima, intensity of Tc I line, ratio of the number of days from minimum to the next following maximum to the period, and infrared colour index [11μ] ? [3.5 μ] are described for S Mira variables.

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Warranty Management and Product ManufactureFor the present conference, the principal interest in studying the distributions and motions of peculiar red giants (in our own and other galaxies) is in the information that this gives us on the population types (ages, masses) and evolutionary phases of these stars.