CaltechAUTHORS
  A Caltech Library Service

An instrument for in situ comet nucleus surface density profile measurement by gamma ray attenuation

Ball, Andrew J. and Gadomski, Stanislaw and Banaszkiewicz, Marek and Spohn, Tilman and Ahrens, Thomas J. and Whyndham, Matthew and Zarnecki, John C. (2001) An instrument for in situ comet nucleus surface density profile measurement by gamma ray attenuation. Planetary and Space Science, 49 (9). pp. 961-976. ISSN 0032-0633. https://resolver.caltech.edu/CaltechAUTHORS:20141027-165633583

Full text is not posted in this repository. Consult Related URLs below.

Use this Persistent URL to link to this item: https://resolver.caltech.edu/CaltechAUTHORS:20141027-165633583

Abstract

The MUPUS experiment on the Rosetta Lander will measure thermal and mechanical properties as well as the bulk density of the cometary material at and just below the surface of the nucleus of comet 46P/Wirtanen. A profile of bulk density vs. depth will be obtained by measuring the attenuation of 662 keV gamma rays emitted by a ^(137)Cs source. Compton scattering is the dominant interaction process at this energy, the attenuation depending directly on the total number of electrons along the source–detector path. This in turn is approximately proportional to the column density. We report here on the design of the bulk density instrument and the results of related Monte Carlo simulations, laboratory tests and calculations of the instrument's performance. The ^(137)Cs radioisotope source is mounted in the tip of the MUPUS thermal probe—a 10 mm diameter rod, to be hammered into the surface of the nucleus to a depth of ~ 370 mm. Two cadmium zinc telluride (CZT) detectors mounted at the top of the probe will monitor the count rate of 662keV photons. Due to the statistics of photon counting, the integration time required to measure column density to a particular accuracy varies with depth as well as with bulk density. The required integration time is minimised for a material thickness equal to twice the exponential attenuation length. At shallower depths the required time rises due to the smaller fractional change in count rate with varying depth, while at greater depths the reduced count rate demands longer integration times. The former effect and the fact that the first 45 mm of the source–detector path passes not through the comet but through the material of the probe, mean that the first density measurement cannot be made until the source has reached a depth of perhaps 100 mm. The laboratory experiments indicate that at this depth an integration time no less than 348 s (falling to 93.9 s at full penetration) would be required to measure a bulk density of 1000 kg m^(-3) to 5% accuracy, assuming a source activity of 1.48 mCi (decayed from an initial 2 mCi). Although solutions involving feedback of the measured bulk density into a time-budgeting algorithm are conceivable, a simple approach where equal time is spent per unit depth may be best, providing an accuracy in bulk density of around 5–20%, for 25 mm slices and the expected range of parameters.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1016/S0032-0633(01)00041-1DOIArticle
http://www.sciencedirect.com/science/article/pii/S0032063301000411PublisherArticle
Additional Information:© 2001 Elsevier Science Ltd. Received 11 December 2000; Accepted 29 January 2001. A.J. Ball acknowledges the postgraduate studentship award provided by the Particle Physics and Astronomy Research Council (PPARC) from 1994–1997, the postdoctoral stipendium provided by the Deutsche Forschungsgemeinschaft (DFG) from 1999–2000, as well as support from the International Space Science Institute (ISSI), while a Junior Visiting Scientist there during 1998. The authors wish to thank the University of Kent’s Unit for Space Sciences and Astrophysics (A.J. Ball and J.C. Zarnecki) and University College London’s Mullard Space Science Laboratory (M. Whyndham and A. Smith) for initial definition and development of this instrument between 1995 and 1997. Thanks also to M.R. Leese (The Open University) for help with procurement of detectors and preamplifiers, M. Hlond (SRC Warsaw) for his work on the software, H. Rickman (Uppsala Astronomical Observatory) and N. Thomas (MPAe Lindau) for discussions on mass, volume and density, and K. Seiferlin (IfP Münster) for feedback on the manuscript.
Funders:
Funding AgencyGrant Number
Particle Physics and Astronomy Research Council (PPARC)UNSPECIFIED
Deutsche Forschungsgemeinschaft (DFG)UNSPECIFIED
International Space Science Institute (ISSI)UNSPECIFIED
Issue or Number:9
Record Number:CaltechAUTHORS:20141027-165633583
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20141027-165633583
Official Citation:Ball, A. J., Gadomski, S., Banaszkiewicz, M., Spohn, T., Ahrens, T. J., Whyndham, M., & Zarnecki, J. C. (2001). An instrument for in situ comet nucleus surface density profile measurement by gamma ray attenuation. Planetary and Space Science, 49(9), 961-976. doi: http://dx.doi.org/10.1016/S0032-0633(01)00041-1
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:50889
Collection:CaltechAUTHORS
Deposited By: Joanne McCole
Deposited On:28 Oct 2014 18:55
Last Modified:03 Oct 2019 07:27

Repository Staff Only: item control page