A Global Geomorphologic Map of Saturn's Moon Titan.

Titan has an active methane-based hydrologic cycle1 that has shaped a complex geologic landscape2, making its surface one of most geologically diverse in the solar system. Despite the different materials, temperatures, and gravity fields between Earth and Titan, many surface features are similar between the two worlds and can be interpreted as products of the same geologic processes3. However, Titan's thick and hazy atmosphere has hindered the identification of geologic features at visible wavelengths and the study of surface composition4. Here we identify and map the major geologic units on Titan's surface using radar and infrared data from the Cassini orbiter spacecraft. Correlations between datasets enabled us to produce a global map even where data sets were incomplete. The spatial and superposition relations between major geologic units reveals the likely temporal evolution of the landscape and gives insight into the interacting processes driving its evolution. We extract the relative dating of the various geological units by observing their spatial superposition in order to get information on the temporal evolution of the landscape. Dunes and lakes are relatively young, while hummocky/mountainous terrains are the oldest on Titan. Our results also show that Titan's surface is dominated by sedimentary/depositional processes with significant latitudinal variation, with dunes at the equator, plains at mid-latitudes and labyrinth terrains and lakes at the poles.

Aortic dissection in children and adolescents with Turner syndrome: risk factors and management recommendations.

There is a general lack of awareness of the risk of aortic dissection in Turner syndrome (TS) from both patients with TS and their physicians. Patients often ignore symptoms for up to 24 h before seeking medical advice, significantly increasing their risk of death. A clinical profile of those at risk of dissection is emerging and includes the presence of congenital heart defects, aortic dilatation and hypertension. MRI has revolutionised the visualisation of cardiovascular anatomy in TS but remains underutilised, especially in children and adolescents, and there is currently little guidance on blood pressure (BP) assessment or hypertension management. Children and adolescents with TS at risk of dissection could be easily identified by timely imaging and BP assessment. This would allow medical management or surgical intervention to be put in place to reduce the risk of this major, and often fatal, complication. Since guidance is lacking, we have reviewed the literature on the risk factors for dissection in TS during childhood and adolescence, and make recommendations on the assessment and management of these patients.

Improvement in symptoms of peripheral arterial disease with sildenafil therapy.

A 57-year-old man presented with symptoms of intermittent claudication and was diagnosed with peripheral arterial disease. He was advised to stop smoking and start a walking programme. He had a background history of hypercholesterolaemia and erectile dysfunction, for which he was taking simvastatin and phosphodiesterase type-5 inhibitor sildenafil, respectively. After starting his exercise programme, he noted that his walking distance was more than doubled on the mornings after taking sildenafil, and he has been using sildenafil primarily for shopping trips since that time. Although this single-patient self-experiment has the potential for placebo confounding, the patient was not led to expect this benefit, and there is evidence that reduced nitric oxide bioactivity plays an important role in the pathophysiology of peripheral arterial disease. Given the biological plausibility of this effect, we feel that a randomised, blinded and placebo-controlled clinical study is warranted to confirm the benefit of phosphodiesterase type-5 inhibitors in peripheral arterial disease.

Observing the NICEties of hypertension management.

National Institute for Health and Clinical Excellence guidance for the clinical management of hypertension, published last year, proposes a step change in UK clinical practice.1 Although broadly helpful, there are some concerns about its implementation. Ambulatory blood pressure monitoring for diagnosis of hypertension, though logical, will place an additional financial burden on primary care at a time of austerity. Home blood pressure measurement may be a more practical option. Previous guidance recommended the used of thiazide diuretics as a first-line treatment option.2 Five years later, the new guidelines propose a major change, with an initial emphasis on the use of calcium channel blockers and angiotensin converting enzyme inhibitors/angiotensin receptor blockers, moving the use of thiazide-like diuretics to a third-line option. In addition, bendroflumethiazide, the mainstay of treatment in the UK over many years, has been replaced with chlortalidone, the starting doses of which are not readily available in this country. Cost-effectiveness analysis and a presumed risk of metabolic disorders has guided the rationale for these changes to the therapeutic algorithm, however this may not be robust. Importantly, unless there are special circumstances, reducing the blood pressure in hypertensive patients is more important than the means used to lower it. In future, it will be important to 'personalise' treatment more effectively and base management on lifetime risk.

Rapid and extensive surface changes near Titan's equator: evidence of April showers.

Although there is evidence that liquids have flowed on the surface at Titan's equator in the past, to date, liquids have only been confirmed on the surface at polar latitudes, and the vast expanses of dunes that dominate Titan's equatorial regions require a predominantly arid climate. We report the detection by Cassini's Imaging Science Subsystem of a large low-latitude cloud system early in Titan's northern spring and extensive surface changes (spanning more than 500,000 square kilometers) in the wake of this storm. The changes are most consistent with widespread methane rainfall reaching the surface, which suggests that the dry channels observed at Titan's low latitudes are carved by seasonal precipitation.

Hyperion's sponge-like appearance.

Hyperion is Saturn's largest known irregularly shaped satellite and the only moon observed to undergo chaotic rotation. Previous work has identified Hyperion's surface as distinct from other small icy objects but left the causes unsettled. Here we report high-resolution images that reveal a unique sponge-like appearance at scales of a few kilometres. Mapping shows a high surface density of relatively well-preserved craters two to ten kilometres across. We have also determined Hyperion's size and mass, and calculated the mean density as 544 +/- 50 kg m(-3), which indicates a porosity of >40 per cent. The high porosity may enhance preservation of craters by minimizing the amount of ejecta produced or retained, and accordingly may be the crucial factor in crafting this unusual surface.

Cassini observes the active south pole of Enceladus.

Cassini has identified a geologically active province at the south pole of Saturn's moon Enceladus. In images acquired by the Imaging Science Subsystem (ISS), this region is circumscribed by a chain of folded ridges and troughs at approximately 55 degrees S latitude. The terrain southward of this boundary is distinguished by its albedo and color contrasts, elevated temperatures, extreme geologic youth, and narrow tectonic rifts that exhibit coarse-grained ice and coincide with the hottest temperatures measured in the region. Jets of fine icy particles that supply Saturn's E ring emanate from this province, carried aloft by water vapor probably venting from subsurface reservoirs of liquid water. The shape of Enceladus suggests a possible intense heating epoch in the past by capture into a 1:4 secondary spin/orbit resonance.

Cassini Imaging Science: initial results on Saturn's rings and small satellites.

Images acquired of Saturn's rings and small moons by the Cassini Imaging Science Subsystem (ISS) during the first 9 months of Cassini operations at Saturn have produced many new findings. These include new saturnian moons; refined orbits of new and previously known moons; narrow diffuse rings in the F-ring region and embedded in gaps within the main rings; exceptionally fine-scale ring structure in moderate- to high-optical depth regions; new estimates for the masses of ring-region moons, as well as ring particle properties in the Cassini division, derived from the analysis of linear density waves; ring particle albedos in select ring regions; and never-before-seen phenomena within the rings.

Cassini Imaging Science: initial results on Phoebe and Iapetus.

The Cassini Imaging Science Subsystem acquired high-resolution imaging data on the outer Saturnian moon, Phoebe, during Cassini's close flyby on 11 June 2004 and on Iapetus during a flyby on 31 December 2004. Phoebe has a heavily cratered and ancient surface, shows evidence of ice near the surface, has distinct layering of different materials, and has a mean density that is indicative of an ice-rock mixture. Iapetus's dark leading side (Cassini Regio) is ancient, heavily cratered terrain bisected by an equatorial ridge system that reaches 20 kilometers relief. Local albedo variations within and bordering Cassini Regio suggest mass wasting of ballistically deposited material, the origin of which remains unknown.

Cassini Imaging Science: initial results on Saturn's atmosphere.

The Cassini Imaging Science Subsystem (ISS) began observing Saturn in early February 2004. From analysis of cloud motions through early October 2004, we report vertical wind shear in Saturn's equatorial jet and a maximum wind speed of approximately 375 meters per second, a value that differs from both Hubble Space Telescope and Voyager values. We also report a particularly active narrow southern mid-latitude region in which dark ovals are observed both to merge with each other and to arise from the eruptions of large, bright storms. Bright storm eruptions are correlated with Saturn's electrostatic discharges, which are thought to originate from lightning.

Thickness of a Europan ice shell from impact crater simulations.

Several impact craters on Jupiter's satellite Europa exhibit central peaks. On the terrestrial planets, central peaks consist of fractured but competent rock uplifted during cratering. Therefore, the observation of central peaks on Europa indicates that an ice layer must be sufficiently thick that the impact events did not completely penetrate it. We conducted numerical simulations of vapor and melt production during cratering of water ice layers overlying liquid water to estimate the thickness of Europa's icy crust. Because impacts disrupt material well beyond the zone of partial melting, our simulations put a lower limit on ice thickness at the locations and times of impact. We conclude that the ice must be more than 3 to 4 kilometers thick.

Galileo at Io: results from high-resolution imaging.

During late 1999/early 2000, the solid state imaging experiment on the Galileo spacecraft returned more than 100 high-resolution (5 to 500 meters per pixel) images of volcanically active Io. We observed an active lava lake, an active curtain of lava, active lava flows, calderas, mountains, plateaus, and plains. Several of the sulfur dioxide-rich plumes are erupting from distal flows, rather than from the source of silicate lava (caldera or fissure, often with red pyroclastic deposits). Most of the active flows in equatorial regions are being emplaced slowly beneath insulated crust, but rapidly emplaced channelized flows are also found at all latitudes. There is no evidence for high-viscosity lava, but some bright flows may consist of sulfur rather than mafic silicates. The mountains, plateaus, and calderas are strongly influenced by tectonics and gravitational collapse. Sapping channels and scarps suggest that many portions of the upper approximately 1 kilometer are rich in volatiles.