Silence on Shangri-La: Attenuation of Huygens acoustic signals suggests surface volatiles
|dc.identifier.citation||Lorenz, R. and Leese, M. and Hathi, B. and Zarnecki, J. and Hagermann, A. and Rosenberg, P. and Towner, M. et al. 2014. Silence on Shangri-La: Attenuation of Huygens acoustic signals suggests surface volatiles. Planetary and Space Science. 90: pp. 72-80.|
Objective. Characterize and understand acoustic instrument performance on the surface of Titan. Methods. The Huygens probe measured the speed of sound in Titan's atmosphere with a 1 MHz pulse time-of-flight transducer pair near the bottom of the vehicle. We examine the fraction of pulses correctly received as a function of time. Results. This system returned good data from about 11 km altitude, where the atmosphere became thick enough to effectively transmit the sound, down to the surface just before landing: these data have been analyzed previously. After an initial transient at landing, the instrument operated nominally for about 10 min, recording pulses much as during descent. The fraction of pulses detected then declined and the transmitted sound ceased to be detected altogether, despite no indication of instrument or probe configuration changes. Conclusions. The most likely explanation appears to be absorption of the signal by polyatomic gases with relaxation losses at the instrument frequency, such as ethane, acetylene and carbon dioxide. These vapors, detected independently by the GCMS instrument, were evolved from the surface material by the warmth leaking from the probe, and confirm the nature of the surface materials as 'damp' with a cocktail of volatile compounds. Some suggestions for future missions are considered.
|dc.title||Silence on Shangri-La: Attenuation of Huygens acoustic signals suggests surface volatiles|
|dcterms.source.title||Planetary and Space Science|
NOTICE: this is the author’s version of a work that was accepted for publication in Planetary and Space Science. Changes resulting from the publishing process, such as peer review, editing, corrections, structural formatting, and other quality control mechanisms may not be reflected in this document. Changes may have been made to this work since it was submitted for publication. A definitive version was subsequently published in Planetary and Space Science, Vol. 90 (2014). DOI: 10.1016/j.pss.2013.11.003