Identification of Possible Interstellar Dust Impact Craters on Stardust Foil I033N,1

Details Identification of Possible Interstellar Dust Impact Craters on Stardust Foil I033N,1 Identification of Possible Interstellar Dust Impact Craters on Stardust Foil I033N,1

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufm.p43a1650a&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #P43A-1650

Physics

[1000] Geochemistry, [1028] Geochemistry / Composition Of Meteorites, [6000] Planetary Sciences: Comets And Small Bodies, [6015] Planetary Sciences: Comets And Small Bodies / Dust

Scientific paper

The Interstellar Dust Collector onboard NASA's Stardust Mission - the first to return solid extraterrestrial material to Earth from beyond the Moon - was exposed to the interstellar dust stream for a total of 229 days prior to the spacecraft's return in 2006 [1]. Aluminum foils and aerogel tiles on the collector may have captured the first samples of contemporary interstellar dust. Interstellar Preliminary Examination (ISPE) focuses in part on crater identification and analysis of residue within the craters to determine the nature and origin of the impacting particles. Thus far, ISPE has focused on nine foils and found a total of 20 craters. The number density of impact craters on the foils exceeds by far estimates made from interstellar flux calculations [2]. To identify craters, foil I1033N,1 was scanned with the Field Museum's Evo 60 Scanning Electron Microscope (SEM) at a resolution of 52 nm/pixel with a 15 kV and 170-240 pA beam. Contamination was monitored according to the ISPE protocol: four 4 μm × 3 μm areas of C layers of different thicknesses on a Stardust-type Al foil were irradiated 20 times for 50 s each, while the C and Al signals were recorded with energy-dispersive X-ray spectroscopy (EDS). The C/Al ratio did not increase after 20 repetitions on each of the four areas. The same experiment repeated 7 months later yielded identical results. Thus, analysis with the SEM results in no detectable contamination. Crater candidates were manually selected from SEM images, then reimaged at higher resolution (17 nm/pixel) in order to eliminate false detections. The foil was then sent to Washington University for Auger Nanoprobe elemental analysis of crater 11_175 (diam. 1.1 μm), and to the Naval Research Laboratory for focused ion beam work and transmission electron microscopy and EDS. Twelve crater candidates (diam. 0.28 - 1.1 μm), both elliptical and circular, were identified. The number density of craters on foil 1033N is 15.8 cm^-2. Auger measurements of crater 11_175 revealed the presence of C, O, Al, Si, a small amount of Na, and possibly Ce and Zn [3] - both components of solar cell cover glass - indicating that this particular crater resulted from a particle that impacted the spacecraft's solar panels. TEM/EDS analysis determined the presence of solar cell glass.

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