SpectralClassificationLab - Spectral Classification I...

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Spectral Classification I. Purpose : The purpose of the Spectral Classification lab was to familiarize ourselves with the study of the chemical and physical nature of the sun and stars. This exercise taught us that the apparent spectral differences arise primarily from variations in temperature or density, and that the vast majority of the stars have quite similar chemical compositions. The lab gave us 30 stars that we had to classify ourselves by using a typical spectrum to compare with. II. Procedure : The lab provided us with an objective-prism spectrogram of a region near Gamma Cygni, which was taken on October 16-17, 1950, with a 24-inch Schmidt telescope of Warner and Swasey Observatory. Our objective was to identify the 30 stars numbered in the spectrogram. First, we started by using the typical spectra provided to get a gauge for the stars. We had to look for things such as the presence or absence of certain lines. We also had to look for the relative density of lines to the background. The typical reasons for classifications are the following: Spectral Class Temperature (K) O - Relatively few absorption lines >25,000 B - Moderate Hydrogen lines 11,000-25,000 A- Very strong hydrogen lines 7,500-11,000 F
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This note was uploaded on 12/22/2010 for the course AST 8716 taught by Professor Reim during the Spring '10 term at University of Southern Maine.

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SpectralClassificationLab - Spectral Classification I...

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