Calibration of relative sensitivity factors for impact ionization detectors with high-velocity silicate microparticles

Fiege, K. and Trieloff, M. and Hillier, Jon K. and Guglielmino, M. and Postberg, F. and Srama, R. and Kempf, S. and Blum, J. (2014) Calibration of relative sensitivity factors for impact ionization detectors with high-velocity silicate microparticles. Icarus, 241 . pp. 336-345. ISSN 0019-1035. (doi:https://doi.org/10.1016/j.icarus.2014.07.015) (The full text of this publication is not currently available from this repository. You may be able to access a copy if URLs are provided)

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Official URL
http://dx.doi.org/10.1016/j.icarus.2014.07.015

Abstract

Impact ionization mass spectrometers, e.g., the Cosmic Dust Analyzer (CDA) onboard the Cassini spacecraft can quantitatively analyze the chemical composition of impacting particles, if the ionization efficiencies of the elements to be quantified are appropriately calibrated. Although silicates are an abundant dust species inside and outside the Solar System, an experimental calibration was not available for elements typically found in silicates. We performed such a calibration by accelerating orthopyroxene dust of known composition with a modified Van de Graaff accelerator to velocities of up to 37.9kms-1 and subsequent analyses by a high resolution impact ionization mass spectrometer, the Large Area Mass Analyzer (LAMA). The orthopyroxene dust, prepared from a natural rock sample, contains ~90% orthopyroxene and ~10% additional mineral species, such as clinopyroxene, spinel, amphibole, olivine and glasses, which are present as impurities within the orthopyroxene, due to inclusion or intergrowth. Hence, the dust material can be regarded as a multi-mineral mixture. After analyses, we find that most particle data cluster at a composition ascribed to pure orthopyroxene. Some data scatter is caused by stochastic effects, other data scatter is caused by the chemically different mineral impurities. Our data indicate that these minor mineral phases can be recognized within a multi-mineral mixture. Here, for the first time, we present experimentally derived relative sensitivity factors (RSFs) for impact ionization mass spectroscopy of silicates, enabling the quantitative determination of the composition of cosmic dust grains. Orthopyroxene data were used to infer RSFs for Na, Mg, Al, Si, Ca, Ti, Fe and K, for particles with radii ranging from 0.04μm to 0.2μm and velocities between 19 and 37.9kms-1, impacting on a Rh-target. © 2014 Elsevier Inc.

Item Type: Article
Additional information: Unmapped bibliographic data: LA - English [Field not mapped to EPrints] J2 - Icarus [Field not mapped to EPrints] AD - Institut für Geophysik und extraterrestrische Physik, Universität Braunschweig, Mendelssohnstr. 3, 38106 Braunschweig, Germany [Field not mapped to EPrints] AD - Institut für Geowissenschaften, Universität Heidelberg, Im Neuenheimer Feld 236, 69120 Heidelberg, Germany [Field not mapped to EPrints] AD - Institut für Raumfahrtsysteme, Universität Stuttgart, Pfaffenwaldring 31, 70569 Stuttgart, Germany [Field not mapped to EPrints] AD - LASP, University of Colorado at Boulder, Boulder, CO 80303, United States [Field not mapped to EPrints] AD - Baylor University, Waco, TX 76706, United States [Field not mapped to EPrints] DB - Scopus [Field not mapped to EPrints] M3 - Article [Field not mapped to EPrints]
Uncontrolled keywords: Cosmochemistry, Experimental techniques, Mineralogy
Subjects: Q Science > QB Astronomy > QB651 Planets, Minor
Divisions: Faculties > Sciences > School of Physical Sciences > Centre for Astrophysics and Planetary Sciences
Depositing User: Giles Tarver
Date Deposited: 10 May 2016 11:04 UTC
Last Modified: 11 May 2016 09:32 UTC
Resource URI: https://kar.kent.ac.uk/id/eprint/55353 (The current URI for this page, for reference purposes)
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