Research about the planetary plasma environment
Introduction to Planetary Plasmas
Beside the commonly known states of matter - the solid, liquid and gaseous phase - there exist more exotic states. One is the plasma state. This is a gas that does not consist only out of neutral particles, but also to a large fraction out of ions and electrons. On earth plasmas can be found in lightning discharges as well as in the ionosphere. They have technological applications in plasma displays and experimental fusion reactors. Since stars also consist of plasma, most of the visible universe is in this state of matter.
Plasma is also quite common in our solar system and present in the interplanetary space or even trapped within the self-generated magnetic fields of several planets. Plasma in the interplanetary space originates primarily from the Sun from where it escapes due to its high pressure, forming the solar wind. The solar wind can interact with the magnetic fields of many planets. Their undisturbed fields can be described in first order as dipolar fields. The region which is dominated by the planetary magnetic field is called the magnetosphere. Its dominating pressure is exerted by the magnetic field and the trapped charged particles within the magnetosphere while in the surrounding interplanetary space the dominant pressure is created by the solar wind. This external pressure compresses the planetary dipolar field at the dayside and forms a long magnetotail on the nightside.
The magnetosphere traps many particles near the planet and, more importantly, shields most of the planet from the solar wind flux. Charged particles in the planetary magnetospheres can originate from different sources and are generated by a large variety of mechanisms. For instance, neutral particles can escape the atmosphere of a planet or can be knocked off its atmosphere or surface of a moon. These particles can be ionized due to UV radiation from the sun or collisions with other particles and also contribute to planetary plasmas.
The magnetospheres of planets in our solar system can therefore be considered as big plasma laboratories with conditions which are not attainable at Earth.
In contrast to the other terrestrial planets Mercury does not have an atmosphere, but it has a relatively weak magnetic field. The strong solar UV radiation leads to photo-chemical escape of ions from Mercury's surface. Also solar wind protons can penetrate through the magnetospheric cusps and sputter ions off the surface. Due to the absence of an ionosphere no significant energy can be stored in the magnetosphere of Mercury such that solar wind disturbances will lead to short time deformations of the magnetosphere.
With plasma instrumentation onboard a spacecraft it is possible to observe the escape of ions from Mercury's surface and analyze surface composition and evolution. Also we can study reconnection processes between solar wind and planetary magnetic fields on very short time scales. For this purpose the Planetary Plasma Group contributes to the plasma instrumentation of the Bepi Colombo Mission to Mercury which is to be launched in 2015. The mission consists of the Japanese Mercury Magnetospheric Orbiter (MMO) that contains a large set of ion, electron and field spectrometers and the European Mercury Planetary Orbiter (MPO) that contains ion and neutral spectrometers.
In contrast to planets like the Earth, Jupiter or Saturn, Venus does not have an intrinsic magnetic field and thus its atmosphere is not protected against the incoming solar wind. However, solar UV radiation ionizes the upper atmosphere creating an ionosphere which in turn interacts with the solar wind ions and the magnetic field carried by the solar wind. This interaction leads to the formation of a magnetosphere: the solar wind magnetic field lines are "folded" around Venus, so the plasma flow is directed around the planet. Depending on the balance between internal pressure (exerted by ionospheric plasma) and external pressure (exerted by solar wind plasma), the positions of ionopause and magnetopause vary in altitude.
The ionosphere is assumed to display two distinct states, "magnetized" and "unmagnetized", depending on the penetration depth of the solar wind magnetic field. Accordingly, the electron transport in the ionosphere changes with varying magnetic field configurations. These aspects are currently being studied by the Planetary Plasma Group at MPS.
Since April 2006, the Venus Express spacecraft is in orbit around Venus. The onboard "Analyzer of Space Plasmas and Energetic Atoms", ASPERA-4, comprises several sensors for in-situ investigation of the Venusian plasma environment and the interactions taking place. The Ion Mass Analyser (IMA) is a mass spectrograph designed to detect ions such as H+, He+ and O+ as well as molecular ions in an energy range between 10 eV/e and 40 keV/e. When Venus Express enters the ionosphere on its trajectory, heavy planetary ions can be analyzed. The Electron Spectrometer (ELS) measures electron densities and energies from 5eV up to 20 keV with a maximum time resolution of 4 seconds. During each orbit of Venus Express, the electron measurements can be used to infer the positions of the bow shock and the ionopause. For the investigation of neutral particles, ASPERA-4 contains the NPI (Neutral Particle Imager) and NPD (Neutral Particle Detector). These instruments measure the flux of energetic neutral atoms with high angular resolution, as well as their masses and energies within a range from 0.1 to 10 keV.
Together with the onboard magnetometer, these instruments yield a large range of information on the dynamical processes taking place in the plasma environment of Venus. Furthermore, the current data can be compared with the measurements of the Pioneer Venus Orbiter (PVO) which investigated the planet Venus between 1980 and 1992, so that long-term variations (e.g. dependence of features on solar activity) can be explored in detail.
Our planet Earth has an intrinsic magnetic field. Charged particles become trapped on these magnetic field lines, forming the Earth's magnetosphere. The impact of solar wind particles causes the lines facing the Sun to be compressed. On the other hand, the magnetic field lines facing away from the Sun get stretched and elongated, forming the Earth's magnetotail.
A number of layers and boundaries can be observed in near-Earth space where the solar wind and Earth's magnetic field meet. The first is the Earth's bow shock created when the supersonic solar wind is suddenly slowed as it approaches the magnetosphere. The edge of the magnetosphere is known as the magnetopause. There are two weak points in Earth's defenses, cusps which occur above the planet's north and south magnetic poles. Particles from the solar wind leak into the magnetosphere towards the Earth along magnetic field lines and cause the auroras.
These regions are explored in great detail by Cluster which delivers data since December 2000. Cluster comprises four identical satellites which fly around the Earth in a tetrahedral configuration. This allows studying small-scale structures of the magnetosphere and its environment in three dimensions. Onboard the Cluster satellites are the Research with Adaptive Particle Imaging Detectors (RAPID) that measure energetic particles in the energy range from 30 keV to 4 MeV. The acceleration mechanisms of energetic particles (particularly reconnection) and their composition in different magnetospheric regions are studied using this instrument. The measurements by RAPID play an important role in understanding of the magnetic storms and substorms.
Similar to Venus the planet Mars does have an ionosphere but no global intrinsic magnetic field. Only in the southern hemisphere of the planet exist strong remnant crustal magnetizations. This leads to a complicated pattern of interaction of the ionosphere of Mars with the solar wind: while in the northern hemisphere a stable ionopause and magnetic barrier is formed, in the southern hemisphere features similar to the Earth cusps can be observed.
The Mars Express spacecraft carries the ASPERA-3 plasma instrument which comprises the ion spectrometer IMA with an energy range of 10 eV up to 40 keV, the electron spectrometer ELS (5 eV to 27 keV) and two neutral atom sensors. Unfortunately no magnetometer was included in the Mars Express payload, but the MARSIS radar instrument allows determining local electron density and total magnetic field at the spacecraft position as well as remote ionospheric density profiles. The mass discrimination by the IMA sensor allows measuring the flow and escape of oxygen ions from the upper ionosphere of Mars. The study of the oxygen escape processes is crucial for the understanding of the evolution of water in the Martian atmosphere. The Planetary Plasma Group investigates all the different features of magnetospheric physics at Mars.
The magnetosphere of Jupiter
Jupiter in many aspects is the most outstanding planet in our solar system. Jupiter is the biggest planet. It also has the fastest rotation period and the largest magnetic moment. The radiation belts of Jupiter are the most intense and the radio emissions are the strongest. Jupiter has the largest moon of the solar system Ganymede, and the strongest source of plasma located deep in the inner magnetosphere, the moon Io. This fascinating solar system body is embedded in a very dynamical plasma and magnetic environment which was encountered by Galileo spacecraft, the first Jupiter orbiting mission.
The Energetic Particles Detector (EPD) is an instrument on board of the Galileo spacecraft designed to measure the characteristics of the charged particles population such as energies, intensities, composition and angular distribution. EPD consists of two detector telescopes: the Low Energy Magnetospheric Measurement System (LEMMS) and the Composition Measurement System (CMS). CMS measures the ion fluxes with discriminating ion species in the energy range from 80 to 1250 keV/nuc. LEMMS observes the electron flux in the energy range between 29 and 884 keV and the species-integrated ion flux between 22 and 12400 keV.
Using the data from EPD instrument and the magnetic field measurements the Planetary Plasma Group at MPS studies the energetic particle population which provides new insights into the dynamics of the Jovian magnetosphere. Particlulary, the relation between the energetic particle characteristics and Jovian auroral emissions, the dynamics of the Jovian magnetotail and its similarity to the terrestrial substorms, the composition of the energetic ion population are investigated.
Saturn has an intrinsic magnetic field that creates the second largest magnetosphere in the solar system. It combines properties of the magnetospheres of Jupiter and Earth. The global configuration resembles Jupiter in that respect that the main plasma source is not external (i.e. the solar wind), but internal (plasma production from Saturn's moons and rings). The fast rotation of the planet provides energy and centrifugally transports the internally produced plasma outwards which creates a pancake shaped magnetosphere. The nature of the internal plasma source has been an open question for a long time. With Cassini it could finally be identified as the water geysers located on the south-pole of the moon Enceladus. Saturn resembles Earth in the respect that the mechanism of the aurora is suggested to be the same as Earth and that the solar wind exerts partial control of several other processes.
Since July 2004 the Cassini spacecraft is orbiting Saturn. Onboard is the Magnetospheric Imaging Instrument (MIMI). It consists of the Charge Energy Mass Spectrometer (CHEMS), the Low Energy Magnetospheric Measurement System (LEMMS) and the Ion Neutral Camera (INCA). While CHEMS can measure intensities and composition of ions with low energies (3 keV/e to 220 keV/e), LEMMS measures intensities of high energetic charged particles (10 keV to several MeV). INCA is able to measure intensities and directions of motion of either ions or energetic neutral atoms (ENA) (7 keV/nuc to 3 MeV/nuc).
One of the research topics of the Planetary Plasma Group at MPS is the study of Saturn's magnetosphere based on in-situ plasma observations and simulations. MIMI data is used to study Saturn's magnetosphere and its dynamic processes in detail. This includes studies on dynamic and steady state plasma transport. Large scale mapping of the particle distributions revealed the existence of a radiation belt that only forms in case of enhanced energetic particle flux of the Sun. MIMI data can also be used for comparison with models or can deliver input parameter for simulations.
The data of the MIMI instrument can also be used to study neutral particles and macroscopic objects. This is possible because these objects can deplete the amount of plasma and energetic particles which are measured by MIMI. By using this fact the discovery of previously unknown new ring arcs around Saturn has been achieved. Such findings could afterwards be correlated with remote observations by Cassini (e.g. the cameras).