Abstract
Nine stars from the Vela Remnant and seven stars in the Eta Carinae complex are examined with CCD spectrograms with high signal-to-noise ratios for data regarding the optical interstellar lines. These data are supplemented by observations of objects with known high-velocity components and substantial interstellar Ti II lines. The CCD spectrograms have signal-to-noise ratios of 100-300, a 2-pixel resolving power of 20,000, and cover features of Na I, Ti II, Ca I, CH(+), and CH in the 3200-4400-A range. The Ca I line confirms the high H density in Vela, and the Ti II lines show evidence of shock-induced grain evaporation. Weak shocks are thought to contribute to the CH(+) component, and a high H I density in some clouds is inferred from the CH line. The high H I density is supported by IUE data on Ca I and on the fine-structure carbon lines. The data point to a significant difference in spectroscopic morphology between the two groups of stars, and the need for theoretical support is underscored.
Published Version
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