Atmospheric Structure and Composition

Strobel, D. F.; Atreya, S. K.; Bézard, Bruno; Ferri, F.; Flasar, F. M.; Fulchignoni, M.; Lellouch, E.; Müller‐Wodarg, I. C. F.

doi:10.1007/978-1-4020-9215-2_10

Cited by 35 publications

(34 citation statements)

References 95 publications

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“…As for Titan, the modeled planet-averaged flux is ∼1 × 10 6 O cm −2 s −1 and 4 × 10 5 (OH+H 2 O) cm −2 s −1 referred to the surface, where the higher O flux is due to the broader radial extent of the O torus (Melin et al 2009;Cassidy & Johnson 2010). Given the external fluxes needed to explain Titan's oxygen compounds ((1−4)×10 6 O atom cm −2 s −1 and ∼2 times more H 2 O, see review in Strobel et al 2009) and the observed plume variability, Enceladus may thus provide adequate O to supply Titan's CO (Hörst et al 2008), but falls short by a factor ∼5-20 for H 2 O.…”

Section: Discussion and Implications For The Source Of Water In Saturmentioning

confidence: 99%

Direct detection of the Enceladus water torus withHerschel

Hartogh

Lellouch

Moreno

et al. 2011

A&A

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Cryovolcanic activity near the south pole of Saturn's moon Enceladus produces plumes of H 2 O-dominated gases and ice particles, which escape and populate a torus-shaped cloud. Using submillimeter spectroscopy with Herschel, we report the direct detection of the Enceladus water vapor torus in four rotational lines of water at 557, 987, 1113, and 1670 GHz, and probe its physical conditions and structure. We determine line-of-sight H 2 O column densities of ∼4 × 10 13 cm −2 near the equatorial plane, with a ∼50 000 km vertical scale height. The water torus appears to be rotationally cold (e.g. an excitation temperature of 16 K is measured for the 1113 GHz line) but dynamically excited, with non-Keplerian dispersion velocities of ∼2 km s −1 , and appears to be largely shaped by molecular collisions. From estimates of the influx rates of torus material into Saturn and Titan, we infer that Enceladus' activity is likely to be the ultimate source of water in the upper atmosphere of Saturn, but not in Titan's.

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Section: Discussion and Implications For The Source Of Water In Saturmentioning

confidence: 99%

Direct detection of the Enceladus water torus withHerschel

Hartogh

Lellouch

Moreno

et al. 2011

A&A

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“…Based on this re sult, for the rest of the sim u la tions we used only one fluid; the one that cor re sponds to Ti tan's rain. It is also the liq uid most likely to be found in Ti tan's rivers (Perron et al, 2006;Atreya et al, 2009;Strobel et al, 2009).…”

Section: The Results Of Short Simulationsmentioning

confidence: 99%

“…At least 5 dif fer ent liq uids are con sid ered (Lunine and Atreya, 2008;Atreya et al, 2009;Strobel et al, 2009;Cordier et al, 2009;Kossacki, 2009, 2012;Lorenz et al, 2010). They are mix tures of light hy dro car bons (meth ane, eth ane, pro pane) and ni tro gen N2 (Ta ble 2).…”

Section: Materials Properties Properties Of Liquidsmentioning

confidence: 99%

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Numerical modelling of sedimentary structures in rivers on Earth and Titan

Misiura

Czechowski

2015

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The dif fer ences in the evo lu tion of rivers on Earth and on Ti tan are in ves ti gated. Dy nam i cal anal y sis of the rivers was performed us ing a nu mer i cal pack age CCHE2D de vel oped by the Na tional Cen ter for Com pu ta tional Hydroscience and En gineer ing, Uni ver sity of Mis sis sippi. The model is based on the Navier-Stokes equa tions for depth-in te grated two-di men sional tur bu lent flow and the three-di men sional con vec tion-dif fu sion equa tion of sed i ment trans port. The model en ables in ves ti gation of the evo lu tion of rivers as a func tion of to tal dis charge and other pa ram e ters of the river. Se ries of short (from one to sev eral hours) and long (up to 67 days) sim u la tions were per formed. We have found that three dif fer ent liq uid hy dro car bons con sid ered for Ti tan's rivers give sim i lar ve loc ity fields. It was also found that the sus pended load is the main means of transport in Ti tan's rivers, while in ter res trial ones, for the same dis charge, the bedload could be of the same or der as sus pended load. More over, we sup pose that for spe cific bound ary con di tions, the evo lu tion of rivers on the Earth pro motes the de vel opment of braided rivers, while for the same con di tions evo lu tion on Ti tan fa vours reg u lar me an der ing rivers.

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“…While the troposphere and lower stratosphere of Titan are basically stable (Strobel et al 2010), Venus's atmospheric conditions are far more varied with at least two stable layers (between 30 and 48 km, and upward of 55 km) separated by layers of instability (Kliore & Patel 1980;Gierasch 1987), while cloud tracking, together with in situ measurements by probes, has detected different wind profiles depending on the altitude and latitude range (Gierasch et al 1997;Hueso et al 2012). As a result, several of the classical atmospheric approximations-such as hydrostatic balance, Boussinesq, or anelasticity-can be applied globally or locally within the cloud region of Venus to study waves other than acoustic or inertia-gravity waves.…”

Section: Introductionmentioning

confidence: 99%

Analytical Solution for Waves in Planets With Atmospheric Superrotation. Ii. Lamb, Surface, and Centrifugal Waves

Peralta

Imamura

Read

et al. 2014

ApJS

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This paper is the second in a two-part study devoted to developing tools for a systematic classification of the wide variety of atmospheric waves expected on slowly rotating planets with atmospheric superrotation. Starting with the primitive equations for a cyclostrophic regime, we have deduced the analytical solution for the possible waves, simultaneously including the effect of the metric terms for the centrifugal force and the meridional shear of the background wind. In those cases where the conditions for the method of the multiple scales in height are met, these wave solutions are also valid when vertical shear of the background wind is present. A total of six types of waves have been found and their properties were characterized in terms of the corresponding dispersion relations and wave structures. In this second part, we study the waves' solutions when several atmospheric approximations are applied: Lamb, surface, and centrifugal waves. Lamb and surface waves are found to be quite similar to those in a geostrophic regime. By contrast, centrifugal waves turn out to be a special case of Rossby waves that arise in atmospheres in cyclostrophic balance. Finally, we use our results to identify the nature of the waves behind atmospheric periodicities found in polar and lower latitudes of Venus's atmosphere.

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Atmospheric Structure and Composition

Cited by 35 publications

References 95 publications

Direct detection of the Enceladus water torus withHerschel

Direct detection of the Enceladus water torus withHerschel

Numerical modelling of sedimentary structures in rivers on Earth and Titan

Analytical Solution for Waves in Planets With Atmospheric Superrotation. Ii. Lamb, Surface, and Centrifugal Waves

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