Impacts on Hubble Space Telescope solar arrays: Discrimination between natural and man-made particles

• Published in: Advances in space research 2005, Vol.35 (7), p.1254-1262
• Main Authors: Kearsley, A.T., Drolshagen, G., McDonnell, J.A.M., Mandeville, J.-C., Moussi, A.
• Format: Article
• Language: English
• Subjects: Analytical electron microscopy; Hubble Space Telescope; Hypervelocity impact; Micrometeoroids; Solar array; Space debris
• ISSN: 0273-1177; 1879-1948
• DOI: 10.1016/j.asr.2005.05.049

A Post-Flight Investigation was initiated by the European Space Agency to analyze impacts on solar arrays of the Hubble Space Telescope (HST), exposed to space for 8.25 years at approximately 600 km altitude. The solar cells deployed during the first Service Mission (SM-1 in December 1993) were retrieved in March 2002 as part of Service Mission 3B (SM-3B). A sub-panel of 2 m 2 was cut from the arrays for subsequent selection and removal of individual solar cells for analysis. Six cells (4.8 × 10 −3 m 2) were surveyed for flux of all craters of sizes greater than 5 microns. Analytical scanning electron microscopy was used to analyse residues in 111 features of 3–4000 micron conchoidal detachment diameter ( D co), examined on 23 solar cells. Eighty three show identifiable residue: 38 are Space Debris impacts and 45 Micrometeoroid impacts. Of the remaining 28, 2 contain residue of ambiguous origin, 1 is probably a minor manufacturing flaw, 1 is obscured by contamination, and 24 are unresolved, lacking recognizable residue. The majority of space debris impacts on the SM-3B cells are less than 80 microns D co, dominated by Al-rich residue, probably of solid rocket motor origin, although three may be due to sodium metal droplet impacts. Three larger features include paint pigment and binder, ferrous alloy, and possible carbon-fibre composite material debris. Micrometeoroid residues are found across the entire crater size range and dominate features of between 100 and 1000 microns, their residues are similar to those found in earlier SM-1 surveys. Fe- and Mg-rich silicates dominate; Fe sulphides are common and there are occasional vesicular Ni- and S-bearing mafic silicates of hydrous phyllosilicate origin. A single sodium aluminosilicate residue and one Fe Ni metal residue were found; as well as enigmatic Mg- and S-bearing residues, all considered as probably of micrometeoroid origin. A few Fe-, O- and C-bearing residues were classified as of ambiguous origin.