The Large- and Small-scale Structure of HVCs

Details The Large- and Small-scale Structure of HVCs The Large- and Small-scale Structure of HVCs

Jan 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004assl..312..145s&link_type=abstract

High Velocity Clouds. Edited by Hugo van Woerden, Kapteyn Institute, Groningen, The Netherlands; Bart P. Wakker, University of W

Astronomy and Astrophysics

Astrophysics

3

Scientific paper

The main question addressed in this chapter is whether or not HVCs have small-scale structure that di ers from that in low-velocity gas and the IVCs. If so, this could make it possible to distinguish HVCs from galactic gas not only by their deviating velocities, but also by their structural characteristics. Further, the physical characteristics derived from the small-scale structure may provide clues to their origin. We find that the core-halo structure that was discovered in the early seventies by Giovanelli, Hulsbosch and others, is typical for all HVCs that have been observed so far. We review some methods to characterize the small-scale structure numerically. These include the autocorrelation function, low- and high-pass filtering, and the concept of fractality. In general, these methods show a tendency for HVCs to have more pronounced small-scale structure than lower-velocity gas. However, the differences are not so pronounced that it is possible to easily distinguish between high- and low-velocity gas.

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