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Title:
Interplanetary dust detected by the Cassini CDA Chemical Analyser
Authors:
Hillier, Jon K.; Green, Simon F.; McBride, Neil; Altobelli, Nicolas; Postberg, Frank; Kempf, Sascha; Schwanethal, James; Srama, Ralf; McDonnell, J. Anthony M.; Grün, Eberhard
Affiliation:
AA(Planetary and Space Sciences Research Institute, The Open University, Walton Hall, Milton Keynes, MK7 6AA, UK), AB(Planetary and Space Sciences Research Institute, The Open University, Walton Hall, Milton Keynes, MK7 6AA, UK), AC(Planetary and Space Sciences Research Institute, The Open University, Walton Hall, Milton Keynes, MK7 6AA, UK), AD(NASA/JPL, 4800 Oak Grove Drive, Pasadena, CA 91101, USA), AE(MPI für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany), AF(MPI für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany), AG(Department of Earth Sciences, The Open University, Walton Hall, Milton Keynes, MK7 6AA, UK), AH(MPI für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany), AI(Planetary and Space Sciences Research Institute, The Open University, Walton Hall, Milton Keynes, MK7 6AA, UK), AJ(MPI für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany; Hawaii Institute of Geophysics and Planetology, University of Hawaii, 1680 East West Road, Honolulu, HI 96822, USA)
Publication:
Icarus, Volume 190, Issue 2, p. 643-654. (Icarus Homepage)
Publication Date:
10/2007
Origin:
ELSEVIER
DOI:
10.1016/j.icarus.2007.03.024
Bibliographic Code:
2007Icar..190..643H

Abstract

During its cruise phase, prior to encountering Jupiter, the Cosmic Dust Analyser (CDA) onboard the Cassini spacecraft returned time of flight mass spectra (TOF MS) of two interplanetary dust particles. Both particles were found to be iron-rich, with possible traces of hydrogen, carbon, nickel, chromium, manganese, titanium, vanadium and minor silicates. Carbon, hydrogen, oxygen and potassium are also present as possible contaminants of the impact target of CDA. Silicates and magnesium do not feature predominantly in the spectra; this is surprising considering the expected dominance of silicate-rich minerals in interplanetary dust particles. The particle masses are 9‑8+55×10 kg and 1.4‑0.8+1.9×10 kg. The corresponding radii ranges for the particles, assuming densities from 7874 2500 kg m‑3 are 0.7 4 μm and 2.6 6.8 μm, respectively. With the same density assumptions the β values (ratio of radiation pressure to gravitational force) are estimated as 0.027 0.21 and 0.016 0.06 respectively, allowing possible orbits to be calculated. The resulting orbits are bound and prograde with semi-major axes, eccentricities and inclinations in the region of 0.3 1.26 AU, 0.4 1.0 and 0 60° for the first particle and 0.8 2.5 AU, 0.2 0.9 and 0 30° for the second. The more probable orbits within these ranges indicate that the first particle is in an Aten-like orbit, whilst the second particle is in an Apollo-like orbit, despite both grains having very similar, predominantly metallic compositions. Other possible orbital solutions for both particles encompass orbits which more closely resemble those of Jupiter-family comets.
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