Dust in the planetary system: Dust interactions in space plasmas of the solar system

Cosmic dust particles are small solid objects observed in the solar planetary system and in many astronomical objects like the surrounding of stars, the interstellar and even the intergalactic medium. In the solar system the dust is best observed and most often found within the region of the orbits of terrestrial planets where the dust interactions and dynamics are observed directly from spacecraft. Dust is observed in space near Earth and also enters the atmosphere of the Earth where it takes part in physical and chemical processes. Hence space offers a laboratory to study dust–plasma interactions and dust dynamics. A recent example is the observation of nanodust of sizes smaller than 10 nm. We outline the theoretical considerations on which our knowledge of dust electric charges in space plasmas are founded. We discuss the dynamics of the dust particles and show how the small charged particles are accelerated by the solar wind that carries a magnetic field. Finally, as examples for the space observation of cosmic dust interactions, we describe the first detection of fast nanodust in the solar wind near Earth orbit and the first bi-static observations of PMSE, the radar echoes that are observed in the Earth ionosphere in the presence of charged dust.     

In‐situ analysis of planetary surfaces by Mössbauer spectroscopy

Iron is one of the key elements in the evolution of the solar system and is highly abundant in terrestrial planets. Its oxidation state reflects the history of the oxidation–reduction reactions on planetary surfaces. The identification of iron mineralogies and the relative abundance of iron oxidation states (2+ and 3+) will contribute to a much deeper understanding of the evolution of planetary bodies and their surfaces. Miniaturized Mössbauer spectrometers are under development primarily for missions to the planet Mars and the Moon, but there is also an interest on using such an instrument for space missions to the planet Venus, comets and asteroids. The instrument MIMOS II developed at TU Darmstadt meets the requirements for space application as low mass (about 500 g), small volume, and low power consumption (about 1 W). The instrument has been tested extensively in the laboratory but also recently in the field mounted on the robotic arm of a prototype Martian Rover under development at JPL/NASA, United States.     

Similarity and diversity in photometric and polarimetric opposition effects of small Solar System bodies

The phase-angle dependences of brightness and polarization of light scattered by atmosphereless Solar System bodies (satellites, asteroids, planetary rings) as well as comets and zodiacal light are analysed on the basis of available ground-based and spacecraft observations. We study similarity and diversity in the photometric and polarimetric opposition effects. The similarity of the brightness and polarization phase functions for polydisperse dust media (cometary and interplanetary dust) and for atmosphereless bodies at small phase angles gives grounds to state that at least some physical properties of dust particles and light-scattering mechanisms should be similar for the two classes of objects. The aggregate structure of particles in different objects can be precisely the property that determines the photometric and polarimetric effects observed in the opposition region. Differences observed in opposition effects for different objects are likely caused by different physical properties (composition, sizes, structure, density) of the scattering particles and, therefore, by different relative contributions of the light-scattering mechanisms. However, the relationship between the photometric opposition effect, spike effect, negative polarization branch, and polarization opposition effect for different bodies is ambiguous.     

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.     

Frozen methanol bombarded by energetic particles: Relevance to solid state astrochemistry

Methanol is an important precursor of many complex prebiotic species and is found abundantly, in solid phase, in several astrophysical environments, such as comets and protostars. These environments are, in general, subjected to some form of ionizing particles as cosmic rays, solar wind particles and/or photons. To simulate physico chemical effects of cosmic rays on methanol and to investigate in particular its fragmentation and cluster emission from the solid phase, condensed methanol at 55 K was bombarded with ∼65 MeV heavy ions constituted by ²⁵²Cf fission fragments. Mass spectra of positive desorbed ions were obtained using a time-of-flight Plasma Desorption Mass Spectrometry (PDMS-TOF), giving information on the fragmentation pattern and abundance of the ionic species released from the frozen sample surface. Since and CH₃O⁺ are the most abundant species detected, the hydrogenation and de-hydrogenation of methanol result to be the predominant ionic processes in the methanol surface. Furthermore, the hydrogenation yields emission of the (CH₃OH)_nCH₃ cluster series, while the CH₃O⁺ species does not attach to methanol molecules. The production of other cluster ion series, some of them with mass/charge up to 300 u/e was also analyzed by PDMS.     

Small-angle scattering and diffraction

The direct measurement of magnetic fields by magnetometers, originally made of the Earth's magnetic field, has been now extended to solar planets by numerous satellite missions. Magnetic effects have been observed in the solar neighborhood and even near some comets, such as the Giotto mission to comet Halley. However, observations of magnetic fields in cosmic objects require remote sensing methods.     

Polarimetry of small bodies of the solar system with large telescopes

During the last 10 years, the FORS instrument of the ESO very large telescope was regularly used to obtain broadband linear polarization measurements of small bodies of the solar system. In particular, FORS was the first (and so far unique) instrument that allowed us to explore polarimetrically objects of the solar system other than planets, moons, asteroids, and active comets. From 2002 to 2010, more than 150 h of telescope time were allocated for the observations of Centaurs, trans-Neptunian objects, and cometary nuclei. With a R magnitude between 16 and 21, these targets are probably the faintest objects of the solar system ever observed in polarimetric mode. In addition to these objects, polarimetric measurements were obtained for asteroids, active comets, Mars, the Saturn moon Iapetus, and the Moon earthshine. Here we present a review of these measurements, from the strategies adopted for the observations to the observational results.     

Danger of the explosion of Callisto and the priority of space missions

Ice is a protonic conductor, as has been demonstrated many times by electrolysis experiments. The dirty ices which comprise the thick (∼10³ km) crusts of several distant moonlike bodies are subjected to bulk electrolysis by currents excited by the motion of such bodies in cosmic magnetic fields (for example, Voyager-1 measured a current amounting to ∼10⁷ A flowing through the Jovian satellite Io and its surroundings). The accumulation of electrolysis products in ice in amount equal to 10–15 wt. % renders such a solid solution capable of detonation. Global explosions of the crusts of moonlike bodies account for the origin and the known properties of many asteroids, short-period comets, planetary rings and small satellites, the formation of Titan’s atmosphere, the differences between Jupiter’s Galilean satellites, etc. Many predictions made on this basis have already been confirmed, and others are awaiting testing. According to all the signs, only the ices of the fourth Galilean satellite Callisto have not yet exploded. If they explode, the Earth will be subjected to concentrated bombardment by cometary nuclei, which will create a “nuclear winter” once every 60 years on the average. Therefore, a very high priority should be assigned to in situ investigations of Callisto for the purpose of determining the degree of saturation of its ices with electrolysis products. Zh. Tekh. Fiz. 69, 10–14 (September 1999)     

Cosmic dust and our origins

The small solid particles in the space between the stars provide the surfaces for the production of many simple and complex molecules. Processes involving the effects of ultraviolet irradiation of the thin (hundredth micron) mantles are shown to produce a wide range of molecules and ions also seen in comets. Some of the more complex ones inferred from laboratory experiments are expected to play an important role in the origin of life. An outline of the chemical evolution of interstellar dust as observed and as studied in the laboratory is presented. Observations of comets are shown to provide substantial evidence for their being fluffy aggregates of interstellar dust as it was in the protosolar nebula, i.e. the interstellar cloud which collapsed to form the solar system. The theory that comets may have brought the progenitors of life to the earth is summarized.     

Formation of Suprathermal Particle Fluxes in a Strongly Turbulent Plasma

We consider the problem on the formation of suprathermal particle fluxes by electrostatic structures in strongly turbulent cosmic plasmas. It is shown that regions with a strong plasma turbulence can be large accelerators of charged particles. We give solutions of the stationary kinetic equation in a turbulent layer for different acceleration regimes and estimate the efficiency of diffusion over the longitudinal and transverse velocities of particles with respect to the magnetic field. The transverse diffusion in velocity space is more efficient for ions and leads to strong isotropization of ion fluxes. Electrons move almost along the magnetic field. We reveal the conditions under which the regular force in a nonuniform magnetic field influences the stochastic-acceleration process. The average energy of axial motion of the particles and the particle fluxes at large distances from the injection region are estimated. Ions and electrons can be accelerated up to comparable energies. We analyze the characteristic features of the motion of the relativistic-particle beams. It is shown that strong plasma turbulence can form particle beams with specific energies. The proposed mechanism is useful for explanation of the properties of energetic particles in cosmic plasmas with magnetic-field-aligned currents, e.g., in high-latitude regions of planetary magnetospheres, force-free configurations of the solar corona, and the solar wind.     

Anomalous cosmic ray carbon and oxygen tracks in CN-Kodak

For observation of low energy cosmic ray particles we used CN-Kodak nuclear track detectors on Cosmos satellites. In solar quiet periods during solar minima conditions the detectors registered anomalous cosmic rays (ACRs). The ACRs are characterized by flux enhancements of several elements and it is known that the carbon enhancement is small compared with that of oxygen. In all of our quiet-time exposures the relation between carbon and oxygen was extremely small (C/O 0.03). But in two quiet-time periods of 14.03.96–11.06.96 and of 15.12.97–14.04.98 we have identified many tracks as carbon in a L–R diagram. As a result the observed C/O ratio appears to be more than 0.5, whereas other experiments show no evidence of enhanced flux of carbon during these periods. The reason for the unexpected response of CN-Kodak is discussed.     

Light scattering in the Solar System: An introductory review

We present a concise survey of light scattering by small particles in the atmospheres and surface layers of various Solar System bodies, comets, the interplanetary medium, and in planetary rings. Current issues and recent developments are emphasized. Special attention is given to experimental and numerical approaches for solving problems of light scattering by non-spherical particles. References to more detailed papers, websites and books are presented. Key areas for further research are pointed out.     

Pulsed laser ablation TOF-MS analysis of planets and small bodies

We are developing miniature time-of-flight mass spectrometers, based on nanosecond pulsed Nd:YAG IR and UV laser ablation, for robotic landed missions to Mars, asteroids, comets, and planetary moons. The goal is to obtain grain-scale and bulk major, minor, and trace composition (both atomic and molecular) from solids, with minimal sample manipulation and preparation. We present here a summary of this effort, focusing on the variety of analyses that could be enabled by pulsed laser ablation for sampling and ionization. We show that a number of geochemical and astrobiological objectives on small bodies or Mars could be addressed with highly simplified mass-spectrometer instrumentation, provided a thorough analysis of the yields of elements and organics to the laser-ablation system is conducted. PACS 07.87.+v; 52.38.Mf; 82.80.Rt     

Impacts of fast meteoroids and a plasma–dust cloud over the lunar surface

The possibility of the formation of a plasma–dust cloud in the exosphere of the Moon owing to impacts of meteoroids on the lunar surface is discussed. Attention is focused on dust particles at large altitudes of ~10–100 km at which measurements were performed within the NASA LADEE mission. It has been shown that a melted material ejected from the lunar surface owing to the impacts of meteoroids plays an important role in the formation of the plasma–dust cloud. Drops of the melted material acquire velocities in the range between the first and second cosmic velocities for the Moon and can undergo finite motion around it. Rising over the lunar surface, liquid drops are solidified and acquire electric charges, in particular, owing to their interaction with electrons and ions of the solar wind, as well as with solar radiation. It has been shown that the number density of dust particles in the plasma–dust cloud present in the exosphere of the Moon is ?10^?8 cm^?3, which is in agreement with the LADEE measurements.     

Eruptive events in the solar atmosphere: new insights from theory and 3-D numerical modelling

Ejections of magnetised plasma from the Sun, commonly known as coronal mass ejections (CMEs), are one of the most stunning manifestations of solar activity. These ejections play a leading role in the Sun–Earth connection, because of their large-scale, energetics and direct impact on the space environment near the Earth. As CMEs evolve in the solar corona and interplanetary space they drive shock waves, which act as powerful accelerators of charged particles in the inner solar system. Some of these particles, known as solar energetic particles (SEPs), can strike our planet, and in doing so they can disrupt satellites and knock out power systems on the ground, among other effects. These particles, along with the intensive X-ray radiation from solar flares, also endanger human life in outer space. That is why it is important for space scientists to understand and predict the ever changing environmental conditions in outer space due to solar eruptive events – the so-called space weather. To enable the development of accurate space weather forecast, in the past three decades solar scientists have been challenged to provide an improved understanding of the physical causes of the CME phenomenon and its numerous effects. This paper summarises the most recent advances from theory and modelling in understanding the origin and evolution of solar eruptive events and related phenomena.     

Mössbauer spectroscopy in space

Nearly 40 years after the discovery of the Mössbauer effect for the first time a Mössbauer spectrometer will leave our planet to explore in situ the surface of another solar system body: the red planet Mars [1]. We are currently developing a miniaturized Mössbauer spectrometer (MIMOS) which is part of the scientific payload of the Russian Mars96 mission, to be launched within the next 2–4 years [2,3]. To fulfill the requirements for a space mission to the planet Mars, all parts of the spectrometer had to be extremely miniaturized and ruggedized to withstand the space flight and Mars environmental conditions. The relevant parts (e.g. drive, detector system, electronics etc.) will be described in more detail and its characteristics compared to standard systems. Because of this new development there now is a growing interest to include a Mössbauer (MB) instrument in future space missions to other solar system bodies as for instance Venus, the terrestrial Moon, and a comet nucleus. Because of extremely different environmental conditions (e.g. nearly zero gravity on the surface of a comet nucleus, high pressure and temperature on the surface of Venus, etc.) different instrument designs and concepts are required for different missions. We will present some ideas for various types of missions, as well as the motivation for using Mössbauer spectroscopy in these cases.     

Fermi-level dependent morphology in photoinduced bond breaking on (1 1 0) surfaces of III-V semiconductors

The morphology of structural changes of InP(1 1 0)-(1 × 1) and GaAs(1 1 0)-(1 × 1) induced by electronic processes following laser excitation has been studied by scanning tunneling microscopy. Surface-vacancy clusters are predominantly formed on n-type surfaces, while isolated anion monovacancies are generated almost exclusively on p-type surfaces. This remarkable Fermi-level effect in the morphology is characterized in terms of a screened Coulomb type interaction between charged surface monovacancies and carriers generated by laser excitation. It is shown that localization of photogenerated valence holes induces electronic bond rupture at surface sites.     

The anomalous spectral dependence of polarization in comets

We have found an anomalous (negative) spectral dependence of polarization for split comet 73P/Schwassmann–Wachmann 3, i.e. polarization degree in the I filter is systematically less (4%) than that in the R filter for both B and C subnuclei of the comet. Earlier we revealed a similar effect for comets 21P/Giacobini–Zinner, C/1999 S4 (LINEAR), and 9P/Tempel 1. Together with comet C/1989 X1 (Austin), for which the similar spectral dependence of polarization was also observed, these comets form a group characterized by some peculiar properties of their dust. Since atypical organic composition is a characteristic feature for all these comets, the anomalous spectral dependence of polarization may indicate specifics of origin of these comets. Really, most of these comets (but not all) originated from the Kuiper Belt. Also, most (but not all) of these comets belong to the group of comets depleted in carbon species in the gas phase, which is typical for comets formed in the giant-planet area of the solar system. On the other hand, all of the comets with negative spectral gradient of polarization have the dust dominated by large particles and most of them belong to the Jupiter family. This may indicate that anomalous spectral dependence of their polarization is a result of their evolution. To identify the reason of anomalous polarization, systematic spectropolarimetric observations of Jupiter-family comets are necessary.