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IAG Planetary Geomorphology Working Group

Featured images for June 2010:

Rectilinear Fluvial Networks on Titan

Images and caption contributed by Devon Burr1, Sarah Drummond1 and Robert Jacobsen2.

1Earth and Planetary Sciences Department and Planetary Geosciences Institute, University of Tennessee Knoxville, USA
2Geology Department, Colorado College, USA

Titan, like Earth, has a solid surface enveloped by a substantial atmosphere. Both atmospheres contain a few mass percent of volatiles - hydrocarbons on Titan, water on Earth - that are close to their triple points. These conditions are conducive to precipitation and runoff, resulting in fluvial processes. At Titan, data from the Cassini-Huygens mission indicate the occurrence of methane rainfall and precipitation runoff [Lunine et al., 2008]. In addition, the Descent Imager and Spectral Radiometer (DISR) on the Huygens probe observed branched lineations interpreted as fluvial valley networks with inset streams formed by flowing methane [Tomasko et al., 2005; Perron et al., 2006]. Additional data from the Cassini orbiter instruments - the Cassini Titan Radar Mapper (RADAR), Imaging Science Subsystem (ISS), and Visible and Infrared Mass Spectrometer (VIMS) - also show networked lineations, interpreted as fluvial networks [e.g., Elachi et al., 2005; Porco et al., 2005; Barnes et al., 2007; Lorenz et al., 2008].

On Earth, regional terrain characteristics determine the network pattern, so identifying drainage patterns can reveal attributes of the terrain [e.g., Howard, 1967] (Image 1). In previous planetary studies, network analysis has proven useful in cases where data resolution is low and surface information, like slope, is limited [Pieri, 1980].



Image 1: Network patterns (Howard, 1967). The implications of some of these patterns are provided in Table 1.





On Titan, on-going fluvial network delineation is likewise proving useful in revealing information about the geology of Titan [Burr et al. 2009]. Through use of a simplified algorithm modified from Ichoku and Chorowicz (1994), a variety of network patterns have been identified (Table 1). Several networks on Titan are rectilinear (e.g., Images 2 and 3). Rectilinear networks, characterized by bends and junction angles near 90 degrees, indicate control of surface flow by subsurface tectonic features. Though tectonism is a common process on icy satellites in the outer Solar System, Titan's thick atmosphere and its associated processes can obscure views of the surface, and previous evidence for tectonism was uncertain (Collins et al. 2010). However, these atmospheric processes, specifically precipitation and fluvial run-off, have revealed evidence for subsurface tectonic structures in the form of rectilinear drainage networks.





Image 2: Subset of Synthetic Aperature Radar image T13 showing fluvial network with evidence of tectonic control by structures trending SW-NE (six red and three blue lines) and NW-SE (four green lines). This network is located at the western end of Xanadu, near 222°E, 10°S











Image 3: Subset of Synthetic Aperature Radar image T59 showing fluvial network with evidence of tectonic control by structures trending NW-SE (red lines) and SW-NE (blue lines). The image subset is located near 210°E, 53°S





Rectilinear networks are also found on Earth. For example, rivers near Yellowstone, Wyoming, USA, exhibit a rectilinear morphology (Image 4). Geologic mapping of the region shows two dominant sets of faults, one set trending NW-SE and one set trending SW-NE. The links in the river network in this region frequently lie along these two trends (Image 4), as a result of control by this tectonic fabric.



Image 4: Aerial view of part of Yellowstone National Park (centered near 44° 40' N, 110° 23' W), showing the right angular bends and junction angles of the Yellowstone river and its tributaries. Predominant link azimuths are NE-SW (red and yellow lines) and NW-SE (blue lines), which mirror local normal faults. The width of the image is 19 kilometers. Image credit: Google Earth.

Continued investigations of Titan fluvial networks should yield additional insights into the factors controlling fluvial runoff. Network analysis provides one mechanism for mapping out the subsurface tectonic patterns on Titan.

Further Reading:

Barnes, J. W., et al. (2007), Near-infrared spectral mapping of Titan's mountains and channels, J. Geophys. Res., 112, E11006, doi:10.1029/2007JE002932. [Abstract]

Burr, D.M., R.E. Jacobsen, D.L. Roth, C.B. Phillips, K.L. Mitchell, D. Viola (2009) Fluvial network analysis on Titan: evidence for subsurface structures and west-to-east wind flow, southwestern Xanadu, Geophys. Res. Lett., 36, L22203, doi:10.1029/2009GL040909. [Abstract]

Cartwright, R. and J.A. Clayton (2009) Geomorphic Analysis of North Polar Channel Networks on Titan, and Implications for Active Tectonics and Persistence of Relief Structures. American Geophysical Union, Fall Meeting 2009, abstract #P51C-1138. [Abstract]

Christiansen, Robert L., 2001,The Quaternary and Pliocene Yellowstone Plateau Volcanic Field of Wyoming, Idaho, and Montana [Abstract], U. S. Geological Survey Professional Paper 729-G. [Map]

Collins, G.C., et al. (2010) Tectonics of the outer planet satellites, in Planetary Tectonics, Cambridge University Press, 530 pages. [Abstract]

Elachi, C., et al. (2005), Cassini radar views the surface of Titan, Science, 308, 970-974, doi:10.1126/science.1109919. [Abstract]

Howard, A. D. (1967), Drainage analysis in geologic interpretation: A summation, Am. Assoc. Pet. Geol. Bull., 51, 2246-2259. [Abstract]

Ichoku, C., and J. Chorowicz (1994), A numerical approach to the analysis and classification of channel network patterns, Water Resources Research, 30(2), 161-174. doi:10.1029/93WR02279. [Abstract]

Lorenz, R., et al. (2008), Fluvial channels on Titan: Initial Cassini RADAR observations, Planet. Space Sci., 56(8), 1132-1144, doi:10.1016/j.pss.2008.02.009. [Abstract]

Lunine, J., et al. (2008), Titan's diverse landscapes as evidenced by Cassini RADAR's third and fourth looks at Titan, Icarus, 195, 415-433, doi:10.1016/j.icarus.2007.12.022. [Abstract]

Perron, J. T., M. P. Lamb, C. D. Koven, I. Y. Fung, E. Yager, and M. Ádámkovics (2006), Valley formation and methane precipitation rates on Titan, J. Geophys. Res., 111, E11001, doi:10.1029/2005JE002602. [Abstract]

Pieri, D. C. (1980), Geomorphology of Martian valleys, in Advances in Planetary Geology, NASA Tech. Memo, TM-81979, 160 pp.

Porco, C. C., et al. (2005), Imaging of Titan from the Cassini spacecraft, Nature, 434, 159-168, doi:10.1038/nature03436. [Abstract]

Tomasko, M. G., et al. (2005), Rain, winds, and haze during the Huygens probe's descent to Titan's surface, Nature, 438, 765-778, doi:10.1038/nature04126. [Abstract]

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