Densities and Mineralogy of Cometary and Asteroidal Interplanetary Dust Particles Collected in the Stratosphere

Details Densities and Mineralogy of Cometary and Asteroidal Interplanetary Dust Particles Collected in the Stratosphere Densities and Mineralogy of Cometary and Asteroidal Interplanetary Dust Particles Collected in the Stratosphere

Jan 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007esasp.643..141j&link_type=abstract

Workshop on Dust in Planetary Systems (ESA SP-643). September 26-30 2005, Kauai, Hawaii. Editors: Krueger, H. and Graps, A., p.1

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Atmospheric entry velocities were estimated on 31 stratospheric IDPs (interplanetary dust particles) using measured atmospheric entry temperatures from stepped He-release release measurements [4] and the atmospheric entry model of Love and Brownlee [5]. Twelve IDPs with atmospheric entry velocities > 18 km/s are believed to have been derived from comets while 4 IDPs with atmospheric entry velocities < 14 km/s likely originated in asteroids. Significant differences in density, morphology and mineralogy exist between the cometary and asteroidal groups. The cometary IDPs have an average density of 1.0 g/cm^3 and are largely dominated by high internal porosities and anhydrous mineralogy. One cometary IDP, which is dissimiliar to the others, is principally composed of hydrated silicate minerals. The asteroidal IDPs have a much higher average density of 3.3 g/cm^3 compared to the cometary IDPs. Three of the four asteroidal IDPs are principally composed of hydrated minerals with low porosities arranged in compact structures. One asteroidal IDP, however, is similar to the majority of cometary IDPs; it contains anhydrous minerals with high internal porosity.

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