New Cassini RADAR results for Saturn’s icy satellites

• Published in: Icarus (New York, N.Y. 1962) Vol. 206; no. 2; pp. 498 - 506
• Main Authors: Ostro, S.J., West, R.D., Wye, L.C., Zebker, H.A., Janssen, M.A., Stiles, B., Kelleher, K., Anderson, Y.Z., Boehmer, R.A., Callahan, P., Gim, Y., Hamilton, G.A., Johnson, W.T.K., Veeramachaneni, C., Lorenz, R.D.
• Format: Journal Article Conference Proceeding
• Language: English
• Published: Amsterdam Elsevier Inc 01-04-2010; Elsevier
• Subjects: Astronomy; Earth, ocean, space; Exact sciences and technology; Radar observations; Satellites, General; Saturn, Satellites; Solar system; Saturn, Satellites; Satellites, General; Radar observations; Iapetus; Tethys; Electrical properties; Backscattering; Light curves; Ice; Regolith; Meteoroids; Dione; Angular diameter; Ammonia; Albedo; Rhea; Asteroids; Correlations; Enceladus; Radar observation; Saturn satellite; Solar system; Asteroid belt
• ISSN: 0019-1035; 1090-2643
• DOI: 10.1016/j.icarus.2009.07.041

Cassini radar tracks on Saturn’s icy satellites through the end of the Prime Mission in 2008 have increased the number of radar albedo estimates from 10 (
Ostro et al., 2006) to 73. The measurements sample diverse subradar locations (and for Dione, Rhea, and Iapetus almost always use beamwidths less than half the target angular diameters), thereby constraining the satellites’ global radar albedo distributions. The echoes result predominantly from volume scattering, and their strength is thus strongly sensitive to ice purity and regolith maturity. The combination of the Cassini data set and Arecibo 13-cm observations of Enceladus, Tethys, Dione, Rhea (
Black et al., 2007), and Iapetus (
Black et al., 2004) discloses an unexpectedly complex pattern of 13-to-2-cm wavelength dependence. The 13-cm albedos are generally smaller than 2-cm albedos and lack the correlation seen between 2-cm and optical geometric albedos. Enceladus and Iapetus are the most interesting cases. We infer from hemispheric albedo variations that the E-ring has a prominent effect on the 13-cm radar “lightcurve”. The uppermost trailing-side regolith is too fresh for meteoroid bombardment to have developed larger-scale heterogeneities that would be necessary to elevate the 13-cm radar albedo, whereas all of Enceladus is clean and mature enough for the 2-cm albedo to be uniformly high. For, Iapetus, the 2-cm albedo is strongly correlated with optical albedo: low for the optically dark, leading-side material and high for the optically bright, trailing-side material. However, Iapetus’ 13-cm albedo values show no significant albedo dichotomy and are several times lower than 2-cm values, being indistinguishable from the weighted mean of 13-cm albedos for main-belt asteroids, 0.15
±
0.10. The leading side’s optically dark contaminant must be present to depths of at least one to several decimeters, so 2-cm albedos can mimic the optical dichotomy; however, it does not have to extend any deeper than that. The fact that both hemispheres of Iapetus look Asteroid-like at 13
cm means that coherent backscattering itself is not nearly as effective as it is at 2
cm. Since Iapetus’ entire surface is mature regolith, the wavelength dependence must involve composition, not structure. Either the composition is a function of depth everywhere (with electrical loss much greater at depths greater than a decimeter or two), or the intrinsic electrical loss of some pervasive constituent is much higher at 13
cm than at 2
cm. Ammonia is a candidate for such a contaminant. If ammonia’s electrical properties do not depend on frequency, and if ammonia is globally much less abundant within the upper one or two decimeters than at greater depths, then coherent backscattering would effectively be shut down at 13
cm, explaining the Asteroid-like 13-cm albedo.