Topography of sinuous rilles in the Harbinger Mountains region of the moon

Abstract

AlistTHct. Five sinuous rules occur in mare basalts in the Harbinger Mountains region of the Moon. Complete and accurate topographic data, now available for the first time, make possible a detailed topographic study of these riiles. Rille length ranges from 12 to 79 km and width from 0.8 to 4.8 km. Depth varies from 100 to 300 m and the rules appear to become shallower to the north. The southern ends of the rilies are characterized by circular to elongate depressions that occur on a 30 km in diameter dome of probable volcanic origin. Longitudinal profiles show that the rille floors have a northward slope of less than one degree. This slope is consistent with the general slope of the surrounding mare surface. Structural studies indicate that slope rather than the regional structural pattern is the dominant factor controlling rille direction. Topographic data lend support to the theory that the rilies were formed as lava channels or tubes.

A volcanic origin for the outflow channels of Mars: Key evidence and major implications

“…1969; Greeley, 1971a,b;Howard et al, 1972;M'Gonigle and Schleicher, 1972;Gornitz, 1973;Young et al, 1973;Schultz, 1976;Greeley and Spudis, 1978;Wilson, 1991, 1992;Leverington and Maxwell, 2004;Leverington, 2006). With channel widths of up tõ 10 km, the largest lunar outflow systems are located in the Aristarchus region of the Moon, and include Vallis Schröteri, Rimae Aristarchus, and Rimae Prinz (e.g., Gornitz, 1973;Schultz, 1976;Strain and El-Baz, 1977;Zisk et al, 1977;Wilhelms, 1987;Campbell et al, 2008) (Fig. 4A).…”

“…4A). Most lunar systems are comprised of simple channels, but some possess attributes that on other solar system bodies might be considered diagnostic of the flow of water, such as inner channels, anastamosing reaches, streamlined erosional residuals, branching channel patterns, and reaches suggestive of lateral or vertical erosion (e.g., Howard et al, 1972;Gornitz, 1973;Carr, 1974;Schultz, 1976;Strain and El-Baz, 1977;Greeley and Spudis, 1978;Wilhelms, 1987;Leverington, 2004Leverington, , 2006Bleacher et al, 2010). The morphologies of lunar channels and numerous mare flows suggest that associated lavas were generally erupted with low yield strengths and at high flow rates (Hulme, 1973;Schaber, 1973;Hulme, 1974;Guest and Murray, 1976;Head, 1976;Schaber et al, 1976;Hulme and Fielder, 1977;Gifford and El-Baz, 1981;Hulme, 1982;Wilson, 1991, 1992;Zimbelman, 1998), and such inferences are consistent with the high iron and titanium contents and low silica content typical of lunar magmas McBirney, 1970, 1973).…”

“…The head depressions of lunar channels are characterized by a wide range of possible forms, with the elongate morphologies of some depressions (e.g., at Rimae Prinz and Rima Hadley) suggesting tectonic control of underlying intrusions (e.g., Gornitz, 1973;Strain and El-Baz, 1977;Leverington, 2009). Channels of relatively limited dimensions (with widths of up to~3 km and lengths of tens to hundreds of kilometers) are most common on the Moon and include systems that head in upland regions (e.g., Rima Hadley, Rimae Plato, and Rimae Maupertuis) and systems that are mostly or entirely confined to mare units (e.g., Rimae Herigonious and Rima Brayley) (e.g., Oberbeck et al, (Baker et al, 1992) is part of the Ammavaru volcanic complex and is over 1000 km long (after Leverington, 2009); flow along this reach was eastward.…”

Volcanic processes as alternative mechanisms of landform development at a candidate crater‐lake site near Tyrrhena Patera, Mars

“…The general morphology of the main inlet channel is notably consistent with that of volcanic rilles on the Earth, Moon, Venus, and Mars. These similarities are consistent on the basis of both overall appearance [ Greeley , 1971a, 1971b; Howard et al , 1972; Young et al , 1973; Guest and Murray , 1976; Zisk et al , 1977; Wilhelms , 1987; Saunders and Pettengill , 1991; Baker et al , 1992, 1997; Head et al , 1992; Komatsu et al , 1992, 1993; Gregg and Greeley , 1993; Komatsu and Baker , 1994; Peterson et al , 1994; Kauahikaua et al , 1998; Leverington and Maxwell , 2004] (Figure 11) and the general form and dimensions of high‐resolution cross‐sectional profiles [ Wu et al , 1972; Swann et al , 1972; Strain and El‐Baz , 1977]. These profiles, particularly with regard to systems such as lunar Rima Hadley, are broadly comparable to those described in section 2 in terms of appearance and width‐to‐depth ratios (Figure 12).…”

“…These profiles, particularly with regard to systems such as lunar Rima Hadley, are broadly comparable to those described in section 2 in terms of appearance and width‐to‐depth ratios (Figure 12). The relatively shallow gradient (<1%) of the main reach of the sinuous inlet channel is also consistent with known lunar volcanic channels [e.g., Strain and El‐Baz , 1977].…”