Latitudinal variations in the solar wind electron heat flux

Ulysses measurements of the solar wind electron heat flux as a function of heliographic latitude are presented. The latitudinal in the electron heat flux presented have been normalized by the radial gradient in the electron heat flux obtained during the in-ecliptic phase of the Ulysses mission (q_e R^–3.0). We find no significant variation in electron heat flux with latitude.     

The Solar Origin of Corotating Interaction Regions and Their Formation in the Inner Heliosphere

Corotating Interaction Regions (CIRs) form as a consequence of the compression of the solar wind at the interface between fast speed streams and slow streams. Dynamic interaction of solar wind streams is a general feature of the heliospheric medium; when the sources of the solar wind streams are relatively stable, the interaction regions form a pattern which corotates with the Sun. The regions of origin of the high speed solar wind streams have been clearly identified as the coronal holes with their open magnetic field structures. The origin of the slow speed solar wind is less clear; slow streams may well originate from a range of coronal configurations adjacent to, or above magnetically closed structures. This article addresses the coronal origin of the stable pattern of solar wind streams which leads to the formation of CIRs. In particular, coronal models based on photospheric measurements are reviewed; we also examine the observations of kinematic and compositional solar wind features at 1 AU, their appearance in the stream interfaces (SIs) of CIRs, and their relationship to the structure of the solar surface and the inner corona; finally we summarise the Helios observations in the inner heliosphere of CIRs and their precursors to give a link between the optical observations on their solar origin and the in-situ plasma observations at 1 AU after their formation. The most important question that remains to be answered concerning the solar origin of CIRs is related to the origin and morphology of the slow solar wind. This revised version was published online in August 2006 with corrections to the Cover Date.     

Cutting force and specific energy for rotary ultrasonic drilling based on kinematics analysis of vibration effectiveness

Rotary ultrasonic drilling(RUD) has become an effective approach for machining advanced composites which are widely using in the field of aeronautics. The cutting kinematics and the corresponding material removal mechanisms are distinct in different drilling areas during RUD. However, these fundamentals have not been fully considered in the existing studies. In this research, two distinct forms of interaction induced by ultrasonic vibration were considered as impact-separation and vibratory lapp...     

Interaction between whistler-mode waves and electrons in the vicinity of interplanetary shocks as seen by Ulysses: A preleminary study

We present a study of wave particle interaction in the vicinity of interplanetary shocks in the ecliptic plane, as observed by the Ulysses spacecraft. We focus here on some events, for which electromagnetic waves are observed, mainly down-stream of the shock. The whistler mode waves are studied by means of the Unified RAdio and Plasma wave experiment (URAP) and the electron distribution functions are obtained from the Ulysses' plasma experiment (SWOOPS). The results are discussed in the light of electron-cyclotron instabilities.     

A particle event at 5 AU and 20° southern latitude from measurements with the EPAC instrument on Ulysses

In November 1992, the Ulysses spacecraft observed a multiple solar particle event and a CME event at 5.2 AU and a heliographic latitude of 20° S which were superimposed to the recurrent corotating interacting region. Distinct particle flux increases caused by these events were observed in all energy channels of the EPAC experiment. The experimental findings are discussed.     

The Cassini Magnetic Field Investigation

The dual technique magnetometer system onboard the Cassini orbiter is described. This instrument consists of vector helium and fluxgate magnetometers with the capability to operate the helium device in a scalar mode. This special mode is used near the planet in order to determine with very high accuracy the interior field of the planet. The orbital mission will lead to a detailed understanding of the Saturn/Titan system including measurements of the planetary magnetosphere, and the interactions of Saturn with the solar wind, of Titan with its environments, and of the icy satellites within the magnetosphere.This revised version was published online in July 2005 with a corrected cover date.     

RPC: The Rosetta Plasma Consortium

The Rosetta Plasma Consortium (RPC) will make in-situ measurements of the plasma environment of comet 67P/Churyumov-Gerasimenko. The consortium will provide the complementary data sets necessary for an understanding of the plasma processes in the inner coma, and the structure and evolution of the coma with the increasing cometary activity. Five sensors have been selected to achieve this: the Ion and Electron Sensor (IES), the Ion Composition Analyser (ICA), the Langmuir Probe (LAP), the Mutual Impedance Probe (MIP) and the Magnetometer (MAG). The sensors interface to the spacecraft through the Plasma Interface Unit (PIU). The consortium approach allows for scientific, technical and operational coordination, and makes optimum use of the available mass and power resources.     

Planar Structuring of Magnetic Fields at Solar Minimum and Maximum

Planar magnetic structures are regions of the solar wind where the magnetic field is oriented parallel to a fixed plane for several hours or more. Discontinuities in the field direction may be encountered during these periods, their surfaces also being parallel to the plane containing the field. A survey of Ulysses magnetic field data returned during 1990–1998 revealed that the solar wind's magnetic field was planar in nature for at least 9% of the time. A survey is presented of planar magnetic structures encountered by Ulysses during two periods when the spacecraft was travelling south from the ecliptic to high southern heliographic latitudes, in 1992–1994 and 1998–2000. The characteristics of the planar magnetic structures encountered during these times of declining and near-maximum solar activity are described, as well as their apparent relationships with interplanetary shocks and heliospheric current sheet crossings. Planar magnetic structures are more common near solar maximum. However, the proportion of structures coinciding with HCS crossings and shocks seems relatively constant. This revised version was published online in August 2006 with corrections to the Cover Date.     

The United Nations Programme on Space Applications: Status and direction for 2010

The United Nations Programme on Space Applications was established in 1971 to assist countries in making full use of the benefits of space technology and its applications for social and economic development. Since its inception the programme has organized numerous training courses, workshops, seminars and conferences and provided funding support for more than 10?000 experts, mainly from developing countries, to participate in those activities. The programme has continuously evolved over four decades, taking into account the latest developments in the field of space activities, to best serve the capacity-building needs of countries and to help ensure that space-based solutions contribute to improving life on Earth. This report describes the status and direction of the UN Programme on Space Applications as recommended for approval by the UN’s Committee on the Peaceful Uses of Outer Space (UNCOPUOS) Scientific and Technical Subcommittee at its 47th session held in Vienna in February 2010.