Modeling variations in near-infrared spectra caused by the coherent backscattering effect

We study a new optical effect, a spectral manifestation of coherent backscattering, which reveals itself as systematic variations in the depth of absorption bands with changing phase angle. We used Cassini VIMS near-infrared spectra of Saturn's icy satellite Rhea in order to identify and characterize the spectral change with phase angle, focusing on the change in the depth of water-ice absorption bands. To model realistic characteristics of the surfaces of icy satellites, which are most likely covered by micron-sized densely packed particles, we perform simulations using a theoretical approach based on direct computer solutions of the macroscopic Maxwell equations. Our results show that this approach can reproduce the observed phase-angle variations in the depth of the absorption bands. The modeled changes in the absorption bands are strongly affected by physical properties of the regolith, especially by the size and packing density of the ice particles. Thus, the phase-angle spectral variations demonstrate a promising remote-sensing capability for studying properties of the surfaces of icy bodies and other objects that exhibit a strong coherent backscattering effect.     

The cooperation between NASA and ASI on the Cassini mission

Summary The updated status of the cooperation between NASA and ASI on the Cassini mission is here presented. This outstanding scientific mission is devoted to study the Saturnian system with a NASA orbiter and a ESA probe. The Italian involvement, managed by the Agenzia Spaziale Italiana (ASI), concerns the design and development of important Cassini Orbiter subsystems. Promotion of the Italian science community's interests and of the national industry's technological capabilities are the rationales for the cooperation. This is an updated version of the contribution presented at San Miniato.     

Shape and gravitational field of the ellipsoidal satellites

The shape and gravitational field of ellipsoidal satellites are studied by using the tidal theory. For ellipsoidal satellites, the following conclusions were obtained: Firstly, in the early stage of the satellite formation, strong tidal friction allowed the satellites move in a synchronous orbit and evolve into a triaxial ellipsoidal shape. Because the tidal potential from the associated primary and the centrifugal potential from the satellite spin are nearly fixed at the surface, the early satellites are the viscoelastic celestial body, and their surfaces are nearly in the hydrostatic equilibrium state. The deformation is fixed in the surface of the satellite. By using the related parameters of primary and satellite, the tidal height and the theoretical lengths of three primary radii of the ellipsoidal satellite are calculated. Secondly, the current ellipsoidal satellites nearly maintain their ellipsoidal shape from solidification, which happened a few billion years ago. According to the satellite shape, we estimated the orbital period and spinning angular velocity, and then determined the evolution of the orbit. Lastly, assuming an ellipsoidal satellite originated in the hydrostatic equilibrium state, the surface shape could be determined by tidal, rotation, and additional potentials. However, the shape of the satellite’s geoid differs from its surface shape. The relationship between these shapes is discussed and a formula for the gravitational harmonic coefficients is presented.     

Chaotic attitude motion of gyrostat statellites in a central force field

The nonlinear attitude motion of gyrostat satellites in a central force field is investigated, with particular emphasis on their long-time dynamic behavior for a wide range of parameters. The numbers of equilibrium solutions, as well as their stability, vary with the rotor speed, and bifurcation diagrams have been obtained. Various dynamic behaviors of gyrostat satcllites, e.g. periodic, quasiperiodic, and chaotic, are studied via the Poincaré map technique. It is shown that the rotor speed has a significant effect on the dynamic behavior of gyrostat satellites.     

Evidence for resonance electron transfer in photon excited X-ray satellite spectra of fluorine compounds

The KαL¹/KαL⁰ intensity ratio of fluorine is measured in five fluorine compounds with a crystal spectrometer. An anomalous reduction of this intensity ratio was observed in KF and SrF₂, which is attributed to resonance electron transfer from the metal ion to the spectator vacancy in the fluorine ion. KαL²/KαL⁰ intensity ratio of fluorine is also measured. The measured relative intensities are compared with the theoretical estimates of Aberg. Formerly RSIC     

Characterization of Salting-Out Processes during CO2-Clathrate Formation Using Raman Spectroscopy: Planetological Application

Clathrate hydrates are particular solids that planetologists study in detail because those solids may be present in several bodies of the solar system, such as Mars, comets, and the icy satellites. The solids are formed by solid H₂O, like common water ice, but adopt open structures with cavities containing gas molecules. Clathrate hydrates are usually stable at relatively low temperature and high pressure, which are the typical conditions present inside these planetary objects. Their interest for astrobiology is that they represent potential sources of liquid water and gases when they decompose. The present work is focused on the crystallization of clathrates in Europa's (icy satellite of Jupiter) interior conditions. We postulate that clathrate hydrates may play an important role in its crust mineralogy and that it can explain some features of the satellite's surface due to their formation/destabilization. An in situ kinetic study by Raman Spectroscopy of the clathrate formation from salty solutions was performed in our laboratory. The chemical composition that we used mimics those obtained from Europa's surface during the Galileo mission. An effect of the salting-out process in the solution was monitored through the clathrate formational path. Our results demonstrate that this process may have geological consequences on Europa and confirm the suitability of Raman spectroscopy for planetary detection of clathrate hydrates and other ices.     

The Absorption Spectrum of UF6, from 2000 to 4200 Å

The absorption spectrum of UF₆ between 3400 and 4200 Å, is well-documented,^(1–3) but the region below 3400 Å has not been studied in any detail. We present here a spectrum of UF₆ between 2000 and 4200 Å that shows significant structure below 3400 Å. The absorption in this region must be observed at very low pressures and relatively short path lengths.     

Lβ2 satellites in the X‐ray emission spectra of elements 72Hf, 73Ta, 74W, 81Tl, 83Bi and 92U

The satellite spectra arising due to the L₃M_x–M_xN_4,5 (x = 1–5) transition array in the X‐ray emission spectra of ₇₂Hf, ₇₃Ta, ₇₄W, ₈₁Tl, ₈₃Bi and ₉₂U have been calculated using available HFS data on K–LM and L–MN Auger transition energies. The agreement between the calculated and measured energies, that between calculated and measured separations in energies and the consideration of the relative probabilities of all the L₃M_x–M_xN_4,5 transitions have been used as the basis for deciding the origin of the satellites. It has been established that two satellites observed in the Lβ₂ region of the X‐ray spectra of various elements, named β₂^I and β₂^II in the order of increasing energy, are mainly emitted by the L₃M_4,5–M_4,5N_4,5 transitions. It is observed that satellite β₂^I in the spectra of elements with ₇₂Hf to ₇₄W has been assigned to the superposition of the ³F₄–³G₅ and ³F₄–³D₃ transitions and must be the most intense one among all these satellites. The same transition has been proved to be the main origin of satellite β₂^II, reported in the element with ₈₁Tl, ₈₃Bi and ₉₂U. Further, satellite β₂^I, reported in the spectra of elements with ₈₁Tl and ₉₂U, has been associated with the transitions ³D₃–³F₄ and ¹D₂–¹F₃. Finally, line β₂^II, reported in the spectra of elements with Z = 72–74, has been assigned to the ¹F₃–¹G₄ and ³P₀–³D₁ transitions. The possible contributions of other transitions of the L₃M_x–M_xN_4,5 (x = 1–5) array having intensities comparable with those of the above transitions, as well as the corresponding lines that have not yet been observed, have also been discussed. Copyright © 2011 John Wiley & Sons, Ltd.     

一种新型的双光束扫描卫星光通信捕获技术

提出了一种基于双光束扫描的卫星光通信捕获技术。使用两束信标光同时对目标卫星所在的不确定区进行扫描,目标卫星在探测到信标光后利用无线电信号向主动方卫星发送应答信号。通过对应答信号所携带信息的计算分析,最终确定目标卫星所在位置,实现捕获。数值仿真计算表明,该方法比传统方法扫描效率提高90%左右。     

Le satellite Encelade source d'ions N dans la magnétosphère de Saturne

The first pass of the Cassini probe in the vicinity of Saturn, above the E-ring, demonstrated a plasma consisting of water group ions (H⁺, O⁺, OH⁺, H₂O⁺) with a small N⁺ ion component (3%). Using a simple model for the transport of magnetospheric ions, we show that the N⁺ ions can be traced back to the Enceladus satellite. Such a result can be explained by the existence in this icy satellite, supposed to be still geologically active, of volatile components such as ammonia NH₃, or by the previous implantation of N⁺ ions of external origin on its surface. To cite this article: M. Bouhram et al., C. R. Physique 6 (2005).