Titlebook: Effects of Mass Loss on Stellar Evolution; IAU Colloquium no. 5 C. Chiosi,R. Stalio Book 1981 D. Reidel Publishing Company, Dordrecht, Holl

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Dimension Reduction and Feature Selectionree-free fluxes. The resultant mass loss rates show a range of only a factor of four. WC stars generally have larger mas loss rates than WN stars, the mean rates being .(WC) = 4.1×10. M.y. and .(WN) = 2.7×10. M.y.. Optical and ultraviolet data have been used to estimate bolometric luminosities for a

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Cytokines

Data Mining for Business Applicationsspectrograms were taken with the image-tube spectrographs of the 1-m and 4-m telescopes at the Cerro Tololo Inter-American Observatory (CTIO). The emulsion was always IIIa-J baked in “forming gas” (N2+H2). The “blue” spectrograms extend from 3600 to 5000 Å at 45 Å mm.; the “red” ones extend from 500

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Guido Cervone,Pasquale Franzeseics of mass loss are discussed with new theoretical calculations of chromospheric line profiles. A general picture of mass loss from cool stars is developed and related to chromospheric and coronal emissions measured by IUE and the HEAO-2 Obgervatory. These winds range in characteristics from the ho

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Using Data Mining for CRM Evaluation, less typical of the spectrum of an M2 supergiant, except for their very great widths; 2) a shell spectrum consisting of P Cygni-type profiles of neutral and singly-ionized metallic lines of very low excitation potential; and 3) asymmetric absorption lines, including H., Hβ, FeI lines of intermediat

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Mass Loss Rates of OB Stars Derived from Infrared Observationstometry of 70 southern OB stars of various luminosity class has been secured. Program stars have been selected, among those bright enough in the infrared to give a suitable photometric accuracy, in order to cover a wide range of spectral types (Fig. 1).