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In the context of the emergence of extra-terrestrial oceanography, we adapted an existing oceanographic model, SLIM (), to the conditions of Titan, a moon of Saturn. The tidal response of the largest southern lake at Titan's surface, namely Ontario Lacus, is simulated. SLIM solves the 2D, depth-averaged shallow water equations on an unstructured mesh using the discontinuous Galerkin finite element method, which allows for high spatial resolution wherever needed. The impact of the wind forcing, the bathymetry, and the bottom friction is also discussed. The predicted maximum tidal range is about 0.56 m in the southern part of the lake, which is more than twice as large as the previous estimates (see Tokano, Ocean Dyn 60:(4) 803-817 (Tokano )). The patterns and magnitude of the current are also markedly different from those of previous studies: the tidal motion is not aligned with the major axis of the lake and the speed is larger nearshore. Indeed, the main tidal component rotates clockwise in an exact period of one Titan day and the tidal currents can reach 0.046 ms close to the shores depending on the geometry and the bathymetry. Except for these specific nearshore regions, the current speed is less than 0.02 ms . Circular patterns can be observed offshore, their rotational direction and size varying along the day. [ABSTRACT FROM AUTHOR]

The results on the aerosol-size spread influence on dissipative instability of aerosol flow in a cold weakly ionized collisional plasma, which were obtained in the first part of this paper [], are used for the Mars (altitudes 70-100 km) and Titan (altitudes 900-1200 km) atmospheric conditions. The threshold charges and characteristic space-time instability scales are quantitatively estimated. [ABSTRACT FROM AUTHOR]

The chemistry of HCNH + in Titan’s atmosphere is not completely understood despite previous experimental and theoretical studies. In response to recent suggestions in the literature, we have searched for specific products of the reactions of HCNH + with H 2, CH 4, C 2H 2, and C 2H 4 using the flowing afterglow-selected ion flow tube technique. We have probed for an association mechanism for reaction with H 2, and associative-H 2 loss for the reactions involving CH 4, C 2H 2, and C 2H 4. In all cases, these reaction mechanisms were found to be inefficient pathways for the depletion of HCNH +. Our ab initio computational studies characterize the structures and energies for these mechanisms and indicate that the proposed pathways are endothermic or possess reaction barriers. We compare our studies to previous experimental and computational work, and we suggest other ion-neutral reactions with HCNH + that have not been included in previous models of Titan’s ionosphere. [ABSTRACT FROM AUTHOR]

Molecular nitrogen, the main component of the modern atmosphere of Titan, may have formed without significant changes in the nitrogen and hydrogen isotopic composition from the clathrate hydrate of ammonia NH · HO, which is the main accreted form of nitrogen. The most preferable transformation mechanism of NH · HO into atmospheric N is its thermal decomposition in the interior of Titan rather than the photochemical decomposition of ammonia in the upper atmosphere of early Titan. The photolysis of ammonia does not lead to a change in the isotopic composition of nitrogen, as all the nitrogen remains in Titan's atmosphere. The photolysis of NH does not lead to a change in the isotopic composition of nitrogen in Titan's atmosphere. Fractionation of hydrogen and nitrogen isotopes during the impacts of comets with Titan does not seem to be significant either. It will be possible to determine the dissociative fractionation factor, the original ratio N/N, and the mass of Titan's original atmosphere when fractionation of nitrogen isotopes in Titan's atmosphere is examined in additional theoretical and experimental studies that take into account processes occurring during the formation of a system of Saturn's satellites. [ABSTRACT FROM AUTHOR]

Voyager's plasma probe observations suggest that there are at least three fundamentally different plasma regimes in Saturn: the hot outer magnetosphere, the extended plasma sheet, and the inner plasma torus. At the outer regions of the inner torus some ions have been accelerated to reach energies of the order of 43 keV. We develop a model that calculates the acceleration of charged particles in the Saturn's magnetosphere. We propose that the stochastic electric field associated to the observed magnetic field fluctuations is responsible of such acceleration. A random electric field is derived from the fluctuating magnetic field – via a Monte Carlo simulation – which then is applied to the momentum equation of charged particles seeded in the magnetosphere. Taking different initial conditions, like the source of charged particles and the distribution function of their velocities, we find that particles injected with very low energies ranging from 0.129 eV to 5.659 keV can be strongly accelerated to reach much higher energies ranging from 22.220 eV to 9.711 keV as a result of 125,000 hitting events (the latter are used in the numerical code to produce the particle acceleration over a predetermined distance). [ABSTRACT FROM AUTHOR]

On the basis of previous ground-based and fly-by information, we knew that Titan's atmosphere was mainly nitrogen, with some methane, but its temperature and pressure profiles were poorly constrained because of uncertainties in the detailed composition. The extent of atmospheric electricity (‘lightning’) was also hitherto unknown. Here we report the temperature and density profiles, as determined by the Huygens Atmospheric Structure Instrument (HASI), from an altitude of 1,400 km down to the surface. In the upper part of the atmosphere, the temperature and density were both higher than expected. There is a lower ionospheric layer between 140 km and 40 km, with electrical conductivity peaking near 60 km. We may also have seen the signature of lightning. At the surface, the temperature was 93.65 ± 0.25 K, and the pressure was 1,467 ± 1 hPa. [ABSTRACT FROM AUTHOR]

Aerosols in Titan's atmosphere play an important role in determining its thermal structure. They also serve as sinks for organic vapours and can act as condensation nuclei for the formation of clouds, where the condensation efficiency will depend on the chemical composition of the aerosols. So far, however, no direct information has been available on the chemical composition of these particles. Here we report an in situ chemical analysis of Titan's aerosols by pyrolysis at 600 °C. Ammonia (NH3) and hydrogen cyanide (HCN) have been identified as the main pyrolysis products. This clearly shows that the aerosol particles include a solid organic refractory core. NH3 and HCN are gaseous chemical fingerprints of the complex organics that constitute this core, and their presence demonstrates that carbon and nitrogen are in the aerosols. [ABSTRACT FROM AUTHOR]

Titan's middle atmosphere is currently experiencing a rapid change of season after northern spring arrived in 2009 (refs 1, 2). A large cloud was observed for the first time above Titan's southern pole in May 2012, at an altitude of 300 kilometres. A temperature maximum was previously observed there, and condensation was not expected for any of Titan's atmospheric gases. Here we report that this cloud is composed of micrometre-sized particles of frozen hydrogen cyanide (HCN ice). The presence of HCN particles at this altitude, together with temperature determinations from mid-infrared observations, indicate a dramatic cooling of Titan's atmosphere inside the winter polar vortex in early 2012. Such cooling is in contrast to previously measured high-altitude warming in the polar vortex, and temperatures are a hundred degrees colder than predicted by circulation models. These results show that post-equinox cooling at the winter pole of Titan is much more efficient than previously thought. [ABSTRACT FROM AUTHOR]

Methane clouds, lakes and most fluvial features on Saturn’s moon Titan have been observed in the moist high latitudes, while the tropics have been nearly devoid of convective clouds and have shown an abundance of wind-carved surface features like dunes. The presence of small-scale channels and dry riverbeds near the equator observed by the Huygens probe at latitudes thought incapable of supporting convection (and thus strong rain) has been suggested to be due to geological seepage or other mechanisms not related to precipitation. Here we report the presence of bright, transient, tropospheric clouds in tropical latitudes. We find that the initial pulse of cloud activity generated planetary waves that instigated cloud activity at other latitudes across Titan that had been cloud-free for at least several years. These observations show that convective pulses at one latitude can trigger short-term convection at other latitudes, even those not generally considered capable of supporting convection, and may also explain the presence of methane-carved rivers and channels near the Huygens landing site. [ABSTRACT FROM AUTHOR]

Titan's stratospheric ice clouds are by far the most complex of any observed in the solar system, with over a dozen organic vapors condensing out to form a suite of pure and co-condensed ices, typically observed at high winter polar latitudes. Once these stratospheric ices are formed, they will diffuse throughout Titan's lower atmosphere and most will eventually precipitate to the surface, where they are expected to contribute to Titan's regolith.Early and important contributions were first made by the InfraRed Interferometer Spectrometer (IRIS) on Voyager 1, followed by notable contributions from IRIS' successor, the Cassini Composite InfraRed Spectrometer (CIRS), and to a lesser extent, from Cassini's Visible and Infrared Mapping Spectrometer (VIMS) and the Imaging Science Subsystem (ISS) instruments. All three remote sensing instruments made new ice cloud discoveries, combined with monitoring the seasonal behaviors and time evolution throughout Cassini's 13-year mission tenure.A significant advance by CIRS was the realization that co-condensing chemical compounds can account for many of the CIRS-observed stratospheric ice cloud spectral features, especially for some that were previously puzzling, even though some of the observed spectral features are still not well understood. Relevant laboratory transmission spectroscopy efforts began just after the Voyager encounters, and have accelerated in the last few years due to new experimental efforts aimed at simulating co-condensed ices in Titan's stratosphere. This review details the current state of knowledge regarding the organic ice clouds in Titan's stratosphere, with perspectives from both observational and experimental standpoints. [ABSTRACT FROM AUTHOR]

The article discusses the atmosphere of Saturn's moon Titan which consists of hydrogen cyanide particles in its southern pole. Titan's atmospheric make-up helps in studying planetary-satellite organic chemistry as it is similar to the atmosphere of early earth. Topics discussed include Titan's atmospheric constituents such as Nitrogen and Methane, hydrogen cyanide cloud, and Cassini, a spacecraft that measures temperature of these regions.

The article discusses the discovery of methane lakes on the northern latitude of Saturn's moon, Titan during the joint NASA/European Space agency Cassini - Huygens mission. Atmosphere skimming revealed impact craters, cryo-volcanoes and river beds like surface features. Findings stresses the fact that Titan is a complex system where the evolution process is similar to the earth's evolutionary process.

Saturn's largest satellite, Titan, has a dense atmosphere of nitrogen with a few per cent of methane. At visible wavelengths its surface is hidden by dense orange-brown smog, which is produced in the stratosphere by photochemical reactions following the dissociation of methane by solar ultraviolet light. The most abundant of the products of these reactions is ethane, and enough of it should have been generated over the life of the Solar System to form a satellite-wide ocean one kilometre deep. Radar observations have found specular reflections in 75 per cent of the surface spots observed, but optical searches for a sun-glint off an ocean have been negative. Here I explain the mysterious absence or rarity of liquid ethane: it condenses onto the smog particles, instead of into liquid drops, at the cold temperatures in Titan's atmosphere. This dusty combination of smog and ethane, forming deposits several kilometres thick on the surface, including the observed dunes and dark areas, could be named ‘smust’. This satellite-wide deposit replaces the ocean long thought to be an important feature of Titan. [ABSTRACT FROM AUTHOR]

The article presents a study by researcher Andrew Coates and colleagues which used Cassini spacecraft to find that charged particles in Saturn moon Titan's atmosphere flowed away from the moon along magnetic field lines, published in a 2015 issue of the journal "Geophysical Research Letters."

An abstract of the article regarding the atmosphere of Titan, the largest moon of the planet Saturn, is presented.