Introduction to stellar winds by Lamers, Cassinelly
By Lamers, Cassinelly
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14 for a full description). Although few people familiar with the details of the HVC phenomenon accepted this idea, it generated a lot of work in trying to understand HVC metallicities, mapping HVC Hα emission and comparing the gas content of the Local Group with that of other galaxy groups (see Chaps. 2, 6, 8, 15). The original proposal by Blitz et al. (1999) seems untenable, but a variant was proposed by Braun & Burton (1999), who singled out the small HVCs as possible Local Group objects, calling these objects “Compact HVCs” (CHVCs).
2003), Sembach et al. (2003) and Savage et al. (2003) in a special issue of the ApJ Supplement (see summary in Ch. 11). The properties of the O vi indicate the presence of hot gas surrounding complex C (Fox et al. 2004) and the Magellanic Stream, suggesting a new kind of Galactic Corona, one much larger (out to at least 50 kpc) than envisioned by Spitzer. In many directions high-velocity O vi absorption without associated high-velocity H i is found, which might represent hot gas in the Local Group.
On the other hand, toward Mrk 876 Murphy et al. 14 solar implied for this HVC by other sightlines. Since N (H i)∼2×1019 cm−2 , N (H) must be >8×1019 cm−2 . Although the model provided by Maloney (1993) predicts N (H)=7×1019 cm−2 for this N (H i), the implied column densities are not inconsistent with the idea that lower values of N (H i) imply higher H+ /H i ratios. A problem, however, is that no Hα emission associated with complex C is observed in the direction of Mrk 876, which is only possible if the H+ is thinly spread over a many kpc (>5) thick layer.