Meteoroids at 1 AU: Dynamic and Properties

Details Meteoroids at 1 AU: Dynamic and Properties Meteoroids at 1 AU: Dynamic and Properties

Dec 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996esasp.392..335m&link_type=abstract

Environment Modelling for Space-based Applications, Symposium Proceedings (ESA SP-392). ESTEC Noordwijk, 18-20 September 1996. E

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Lines of evidence from both retrieved spacecraft and meteoroid studies have been examined to define the properties and understanding of the particulate impact environment at 1 AU. Key studies include:
From LDEF and Eureca experiments comprising both thin foils and thick targets, exposed under identical exposures, have permitted physical properties of the meteoroids to be deduced such as shape factor and density.
Comparison of such detectors pointing in different directions on the same spacecraft permits the velocity of meteoroids to be assessed and compared with that of radar meteoroids. Results are compared with velocity distributions currently used for ESABASE.
Comparison of science experiments exposed on LDEF and Eureca, where different altitude stabilisation configurations apply, leads to a measure for the upper limit of space debris without recourse to chemical analyses.
Radar meteoroids provide the only effective measure of the velocity distribution at 1 AU; but the meteor phenomenon differs (in sensitivity to velocity) from the impact cratering. Modelling has been performed, therefore, to derive Apex to Anti-Apex flux distributions appropriate to spacecraft environment modelling as in e.g. ESABASE.
High sensitivity in-situ detectors in deep space, in particular HEOS II and Pioneers 8 and 9, provide evidence of the changing distributions and directivity of meteoroids and a swing to beta meteoroids which are being expelled from the solar system. Advances in the characterisation of these populations are presented.

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