Abstract
The principal methods for establishing the chemical composition, long-range structure, short-range structure and nature of chemical bonding at the S-G interface are reviewed. Electron and ion spectroscopies largely developed over the past two decades have vastly improved our ability to establish the interface chemical composition, and developments over the past 5 years have done much to put the determination of long-range and short-range structures on firm ground. The high vacuum requirements of these techniques limit their applications to interfaces whose stability under evacuation can be reasonably presumed. This is a serious limitation for many solar applications, and new methods of characterization not subject to it are urgently needed. Some possibilities are indicated.
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