Planetary X-ray fluorescence analogue laboratory experiments and an elemental abundance algorithm for C1XS |
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| Authors: | Shoshana Z. Weider Bruce M. Swinyard Barry J. Kellett Chris J. Howe Katherine H. Joy Ian A. Crawford Jason Gow David R. Smith |
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| Affiliation: | aDepartment of Earth and Planetary Sciences, Birkbeck College, Malet Street, London WC1E 7HX, UK;bCentre for Planetary Sciences at UCL/Birkbeck, Department of Earth Sciences, Gower Street, London WC1E 6BT, UK;cRAL Space, Rutherford Appleton Laboratory, Didcot, Oxon OX11 0QX, UK;dDepartment of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Road, Washington DC 20015, USA;eDepartment of Physics and Astronomy, UCL, Gower Street, London WC1E 6BT, UK;fCenter for Lunar Science and Exploration, The Lunar and Planetary Institute, USRA, 3600 Bay Area Blvd, Houston, TX 77058, USA;gThe NASA Lunar Science Institute, USA;he2v centre for electronic imaging, PSSRI, The Open University, Milton Keynes, MK7 6AA, UK;iCentre for Sensors and Instrumentation, School of Engineering and Design, Brunel University, Uxbridge, Middlesex, UB8 3PH, UK |
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| Abstract: | We have conducted laboratory experiments as an analogue to planetary XRF (X-ray fluorescence) missions in order to investigate the role of changing incidence (and phase) angle geometry and sample grain-size on the intensity of XRF from regolith-like samples. Our data provide evidence of a grain-size effect, where XRF line intensity decreases with increasing sample grain-size, as well as an almost ubiquitous increase in XRF line intensity above incidence angles of ∼60°. Data from a lunar regolith simulant are also used to test the accuracy of an XRF abundance algorithm developed at the Rutherford Appleton Laboratory (RAL), which is used to estimate the major element abundance of the lunar surface from Chandrayaan-1 X-ray Spectrometer (C1XS) XRF data. In ideal situations (i.e., when the input spectrum is well defined and the XRF spectrum has a sufficient signal to noise ratio) the algorithm can recover a known rock composition to within 1.0 elemental wt% (1σ). |
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| Keywords: | X-ray fluorescence (XRF) spectroscopy Planetary analogues Moon, Mercury, asteroids&mdash surface Regolith Chandrayaan-1 |
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