Study of distribution functions of interplanetary particles accelerated at co-rotating interaction region at∼5A.U.

We report the results of a study of the 12-hour average distribution functions of high Z nuclei as measured over a 10-day interval on the Ulysses spacecraft at a helioradius of5.2 A.U. We use the good time and atomic mass resolution of the composition aperture of the HI-SCALE instrument to determine the form of the distribution functions for C, O, Ne, Mg, Si, and Fe over the energy range 0.5–16 MeV/nucl. We find that the distribution functions of these ions can be organized by characteristic velocities that have values ranging between2000–3500 km/sec over this interval.     

The gradual acceleration of the outflow of VX-Sagittarii: A stellar evolutionary effect?

VX-Sagittarii is a red supergiant with a superwind which is observed in several maser lines. They provide an evidence that the outflow velocity keeps growing considerably at large distance from the star. It is argued that this phenomenon can be explained by stellar evolutionary effects.As a rule, the outflow velocity for late type stars correlates with the mass loss rate and from that it is suggested that the mass loss rate was higher in the past and is decreasing now. The mass of VX Sagittarii can be estimated on this basis and is about 40–50M      

The Application of Overstress Testing-to-Failure to Airborne Electronics?A Status Report

Several years of study and actual testing have answered many of the previously controversial questions about the application of environmental overstress testing-to-failure as a useful tool for reliability evaluation. The answers included the fact that more than 65 percent of the failures occurring under overstress environments were duplicates of experienced operational failures. Improvements of 5 to 1 in reliability levels have resulted from application of results of overstress tests, which consumed less than 200 hours of actual test time. Overstress tests have also been used as a method of evaluating multiplesource designs. The first in a required series of indices has been derived, which may assist in the eventual use of overstress testing for reliability index measurement.     

A hybrid original approach for prediction of the aerodynamic coe?cients of an ATR-42 scaled wing model

A new approach for the prediction of lift, drag, and moment coefficients is presented. This approach is based on the support vector machines (SVMs) methodology and an optimization meta-heuristic algorithm called extended great deluge (EGD). The novelty of this approach is the hybridization between the SVM and the EGD algorithm. The EGD is used to optimize the SVM parameters. The training and validation of this new identification approach is realized using the aerodynamic coefficients of an ATR-42 wing model. The aerodynamic coefficients data are obtained with the XFoil software and experimental tests using the Price–Pa?doussis wind tunnel. The predicted results with our approach are compared with those from the XFoil software and experimental results for different flight cases of angles of attack and Mach numbers. The main pur-pose of this methodology is to rapidly predict aircraft aerodynamic coefficients.     

Large-scale Bright Fronts in the Solar Corona: A?Review of?��EIT waves��

??EIT waves?? are large-scale coronal bright fronts (CBFs) that were first observed in 195 Å images obtained using the Extreme-ultraviolet Imaging Telescope (EIT) onboard the Solar and Heliospheric Observatory (SOHO). Commonly called ??EIT waves??, CBFs typically appear as diffuse fronts that propagate pseudo-radially across the solar disk at velocities of 100?C700 km?s^?1 with front widths of 50?C100 Mm. As their speed is greater than the quiet coronal sound speed (c _s ??200 km?s^?1) and comparable to the local Alfvén speed (v _A ??1000 km?s^?1), they were initially interpreted as fast-mode magnetoacoustic waves ( $v_{f}=(c_{s}^{2} + v_{A}^{2})^{1/2}$ ). Their propagation is now known to be modified by regions where the magnetosonic sound speed varies, such as active regions and coronal holes, but there is also evidence for stationary CBFs at coronal hole boundaries. The latter has led to the suggestion that they may be a manifestation of a processes such as Joule heating or magnetic reconnection, rather than a wave-related phenomena. While the general morphological and kinematic properties of CBFs and their association with coronal mass ejections have now been well described, there are many questions regarding their excitation and propagation. In particular, the theoretical interpretation of these enigmatic events as magnetohydrodynamic waves or due to changes in magnetic topology remains the topic of much debate.