Clutter Residues of a Coherent MTI Radar Receiver

In moving target indicator radar receivers a saturation is always present in the IF stages in order to compress the dynamic range of large clutter inputs. This nonlinearity greatly affects the performances of the cancelling circuits, because of the spreading of the spectra. A quantitative analysis of this effect has been conducted, with an analytical expression chosen for the limitation characteristic. A high degradation of both single-and double-canceller improvement factors has been obtained. Losses of 20 dB for the double canceller are not uncommon. Clutter residue levels at the receiver output have also been computed in order to see how the performance compares with ideal constant false alarm rate behavior.     

Precise Attitude Stabilization of a Large Orbiting Telescope Coupled to a Crew Compartment

Computer simulation results are presented for the planar equations of motion of an attitude-stabilized orbiting telescope passively coupled to a manned service module. This coupling is provided through a set of soft springs and a two-axis gimbal aligned with the telescope center of mass. Principal nonlinearities in the suspension system and the telescope control system are included. The simulation indicates preliminary nary feasibility of this operational mode.     

Stability Measurement Problems and Techniques for Operational Airborne Pulse Doppler Radar

In the deployment of pulse Doppler (PD) radar, determination of phase and amplitude stability is the most difficult measurement problem. Unique requirements are placed on pulse and carrier stability so that the radar can perform in strong clutter. Because of subclutter visibility and sensitivity specifications, coherent noise, which is insignificant for noncoherent pulse radars, becomes extremely important. In solving the measurement problem, special support equipment was developed which is considered to have reached such a degree of refinement that it is probably one of the most technically advanced pieces of field test equipment supporting any operational radar. This paper discusses stability requirements, sources of instability, and the combination of techniques selected for verification of compliance of the PD radar with the stability requirements. The results of a program to develop special field support equipment to satisfy the measurement requirements are emphasized. Results of field experience and the special training required of military field personnel to enable them to effectively use this relatively complex support equipment are discussed.     

Determining total ozone content in the atmosphere using satellite measurements

In this paper a simple method is presented which is applicable for fast determination of total ozone content in the earth atmosphere by using IR radiation intensity data from satellite measurements. The method is based on the property that transmittance of inhomogeneous atmosphere in the 9.6 μm band can be well approximated by the transmittance of a homogeneous ozone slab characterized by its effective pressure and temperature. The effective pressure and temperature were determined as mean values weighted by the average ozone profile of each season. The transmission functions were computed from an empirical formula. Free parameters in the formula were determined by a multiple regression scheme, on the basis of the transmittance data either measured in the laboratory or evaluated by computations using a line by line integration procedure. The main advantage of the described method is an easy and fast computation procedure. According to comparison with direct ozone sounding the accuracy is good enough: the average relative error lies between 5 and 7%.     

The Dynamic Quasiperpendicular Shock: Cluster Discoveries

The physics of collisionless shocks is a very broad topic which has been studied for more than five decades. However, there are a number of important issues which remain unresolved. The energy repartition amongst particle populations in quasiperpendicular shocks is a multi-scale process related to the spatial and temporal structure of the electromagnetic fields within the shock layer. The most important processes take place in the close vicinity of the major magnetic transition or ramp region. The distribution of electromagnetic fields in this region determines the characteristics of ion reflection and thus defines the conditions for ion heating and energy dissipation for supercritical shocks and also the region where an important part of electron heating takes place. In other words, the ramp region determines the main characteristics of energy repartition. All these processes are crucially dependent upon the characteristic spatial scales of the ramp and foot region provided that the shock is stationary. The process of shock formation consists of the steepening of a large amplitude nonlinear wave. At some point in its evolution the steepening is arrested by processes occurring within the shock transition. From the earliest studies of collisionless shocks these processes were identified as nonlinearity, dissipation, and dispersion. Their relative role determines the scales of electric and magnetic fields, and so control the characteristics of processes such as ion reflection, electron heating and particle acceleration. The determination of the scales of the electric and magnetic field is one of the key issues in the physics of collisionless shocks. Moreover, it is well known that under certain conditions shocks manifest a nonstationary dynamic behaviour called reformation. It was suggested that the transition from stationary to nonstationary quasiperiodic dynamics is related to gradients, e.g. scales of the ramp region and its associated whistler waves that form a precursor wave train. This implies that the ramp region should be considered as the source of these waves. All these questions have been studied making use observations from the Cluster satellites. The Cluster project continues to provide a unique viewpoint from which to study the scales of shocks. During its lifetime the inter-satellite distance between the Cluster satellites has varied from 100 km to 10000 km allowing scientists to use the data best adapted for the given scientific objective. The purpose of this review is to address a subset of unresolved problems in collisionless shock physics from experimental point of view making use multi-point observations onboard Cluster satellites. The problems we address are determination of scales of fields and of a scale of electron heating, identification of energy source of precursor wave train, an estimate of the role of anomalous resistivity in energy dissipation process by means of measuring short scale wave fields, and direct observation of reformation process during one single shock front crossing.     

Long-Term Evolution of the Martian Crust-Mantle System

Lacking plate tectonics and crustal recycling, the long-term evolution of the crust-mantle system of Mars is driven by mantle convection, partial melting, and silicate differentiation. Volcanic landforms such as lava flows, shield volcanoes, volcanic cones, pyroclastic deposits, and dikes are observed on the martian surface, and while activity was widespread during the late Noachian and Hesperian, volcanism became more and more restricted to the Tharsis and Elysium provinces in the Amazonian period. Martian igneous rocks are predominantly basaltic in composition, and remote sensing data, in-situ data, and analysis of the SNC meteorites indicate that magma source regions were located at depths between 80 and 150 km, with degrees of partial melting ranging from 5 to 15 %. Furthermore, magma storage at depth appears to be of limited importance, and secular cooling rates of 30 to 40 K?Gyr^?1 were derived from surface chemistry for the Hesperian and Amazonian periods. These estimates are in general agreement with numerical models of the thermo-chemical evolution of Mars, which predict source region depths of 100 to 200 km, degrees of partial melting between 5 and 20 %, and secular cooling rates of 40 to 50 K?Gyr^?1. In addition, these model predictions largely agree with elastic lithosphere thickness estimates derived from gravity and topography data. Major unknowns related to the evolution of the crust-mantle system are the age of the shergottites, the planet’s initial bulk mantle water content, and its average crustal thickness. Analysis of the SNC meteorites, estimates of the elastic lithosphere thickness, as well as the fact that tidal dissipation takes place in the martian mantle indicate that rheologically significant amounts of water of a few tens of ppm are still present in the interior. However, the exact amount is controversial and estimates range from only a few to more than 200 ppm. Owing to the uncertain formation age of the shergottites it is unclear whether these water contents correspond to the ancient or present mantle. It therefore remains to be investigated whether petrologically significant amounts of water of more than 100 ppm are or have been present in the deep interior. Although models suggest that about 50 % of the incompatible species (H₂O, K, Th, U) have been removed from the mantle, the amount of mantle differentiation remains uncertain because the average crustal thickness is merely constrained to within a factor of two.     

The Solar Energetic Particle Ionic Charge Analyzer (SEPICA) and the Data Processing Unit (S3DPU) for SWICS,SWIMS and SEPICA

The Solar Energetic Particle Ionic Charge Analyzer (SEPICA) is the main instrument on the Advanced Composition Explorer (ACE) to determine the ionic charge states of solar and interplanetary energetic particles in the energy range from ≈0.2 MeV nucl−1 to ≈5 MeV charge−1. The charge state of energetic ions contains key information to unravel source temperatures, acceleration, fractionation and transport processes for these particle populations. SEPICA will have the ability to resolve individual charge states and have a substantially larger geometric factor than its predecessor ULEZEQ on ISEE-1 and -3, on which SEPICA is based. To achieve these two requirements at the same time, SEPICA is composed of one high-charge resolution sensor section and two low- charge resolution, but large geometric factor sections. The charge resolution is achieved by the focusing of the incoming ions, through a multi-slit mechanical collimator, deflection in an electrostatic analyzer with a voltage up to 30 kV, and measurement of the impact position in the detector system. To determine the nuclear charge (element) and energy of the incoming ions, the combination of thin-window flow-through proportional counters with isobutane as counter gas and ion-implanted solid state detectors provide for 3 independent ΔE (energy loss) versus E (residual energy) telescopes. The multi-wire proportional counter simultaneously determines the energy loss ΔE and the impact position of the ions. Suppression of background from penetrating cosmic radiation is provided by an anti-coincidence system with a CsI scintillator and Si-photodiodes. The data are compressed and formatted in a data processing unit (S3DPU) that also handles the commanding and various automatted functions of the instrument. The S3DPU is shared with the Solar Wind Ion Charge Spectrometer (SWICS) and the Solar Wind Ion Mass Spectrometer (SWIMS) and thus provides the same services for three of the ACE instruments. It has evolved out of a long family of data processing units for particle spectrometers. This revised version was published online in June 2006 with corrections to the Cover Date.     

Anomalous Cosmic Rays

We review the observed properties of anomalous cosmic rays and the present status of our knowledge of the processes by which they originate. We compiled a comprehensive set of ACR energy spectral data from various spacecraft throughout the heliosphere during the passes of Ulysses over the poles of the Sun and present first results of a detailed modeling effort. In several contributions, we discuss the questions of injection and possible pre-acceleration of pickup ions, summarize new observations on the ionic charge composition, and present new results on the composition of minor ions in ACRs.     

TWA800 fuel tank flammability-an analytical investigation

The mission was to identify the conditions of atmospheric pressure and ambient temperature under which a so-called empty-fuel-tank, containing residual fuel, could contain hazardous air/fuel mixtures. The issues are limited to two applications: explosion safety concerns in gasoline fueled automotive vehicles and explosion safety in jet fueled jet aircraft. In general, we concluded that flammable mixtures, under certain conditions, may exist in an empty fuel tank containing residual fuel, at ambient temperatures ranging from -51°C (-60°F) through 93°C (200°F), at or below atmospheric pressure. However, in the case of a gasoline automotive fuel tank, at normal ambient temperatures above -18°C (0°F), it is absolutely certain that the fuel tank head space contains an over-rich mixture, which cannot explode, unless the automotive fuel tank is completely drained of liquid fuel. Further, in the case of a fixed wing jet aircraft, a combustible mixture also does not exist in a fuel tank containing JetA type fuel at ambient temperatures below 38°C (100°F) which is about the lean limit flash point for commercial jet fuel at sea level. Nevertheless, this study identified six highly unlikely, but rationally possible critical conditions which can occur in a combination which may permit a combustible mixture to exist within a jet aircraft fuel tank and pose a potential hazard. While the scope of this summary paper is limited to fixed wing jet aircraft fuels, details of the automotive vehicle gasoline fueled application are contained in the original paper