[1] It took the solar polar passage of Ulysses in the early 1990s to establish the global structure of the solar wind speed during solar minimum. However, it remains unclear if the solar wind is composed of two distinct populations of solar wind from different sources (e.g., closed loops which open up to produce the slow solar wind) or if the fast and slow solar wind rely on the superradial exp...

EISCAT observations of interplanetary scintillation have been used to measure the velocity of the solar wind at distances between 15 and 130 Rx (solar radii) from the Sun. The results show that the solar wind consists of two distinct components, a fast stream with a velocity of &800 km s~1 and a slow stream at &400 km s~1. The fast stream appears to reach its final velocity much closer to the S...

Simultaneous observations of the solar wind velocity as measured at the Pioneer 9 and Ogo 5 spacecraft during five solar rotations in 1968 and 1969 are presented. During this time, Pioneer 9 was traveling in toward the sun to approximately 0.7 AU while the earth orbiter Ogo 5 was spending long periods in the interplanetary medium. A comparison of the 3-hour averages of solar wind velocity obtai...

The 3-D structure of the solar wind varies dramatically along the Sun’s activity cycle. In the present paper we focus on some properties of the polar solar wind. This is a fast, teneous, and steady flow (as compared to low-latitude conditions) that fills the high-latitude heliosphere at low solar activity. The polar wind has been extensively investigated by Ulysses, the first spacecraft to perf...

While the fast solar wind is nerally thought to originate from coronal holes, the ~, Oa% source of the slow solar wind is only known to be associated with the highly structured and — highly variable streamer belt. There is growing evidence from multiple-station intensity scintillation measurements of solar wind velocity — usually referred to as IPS for interplanetary scintillation— that the slo...

A kinetic model of the solar wind based on Kappa velocity distribution functions for the electrons and protons escaping out of the corona is presented. The high velocity particles forming the tail of these distribution functions have an enhanced phase space density compared to a Maxwellian. The existence of such velocity distribution functions have been introduced in the pioneering work of Scud...

Building integrated photovoltaic/thermal (BIPV/T) systems serve two purposes – generate electricity and heat ambient air using absorbed solar energy. High wind velocity reduces the efficiency of unglazed transpired solar collectors (UTC). Indeed, wind flow on the collector’s surface reduces the useful heat transferred to the plenum air by effectuating convection losses and suction in the pores;...

background: recently, we introduced solar related geomagnetic disturbances (gmd) as a potential environmental risk factor for multiple sclerosis (ms). the aim of this study was to test probable correlation between solar activities and gmd with long-term variations of ms incidence. methods: after a systematic review, we studied the association betwee n alterations in the solar wind velocity (vsw...

[1] We present techniques for comparing measurements of velocity, temperature, and density with constraints imposed by the plasma physics of magnetized bi-Maxwellian ions. Deviations from these physics-based constraints are interpreted as arising from measurement errors. Two million ion spectra from the Solar Wind Experiment Faraday Cup instruments on the Wind spacecraft are used as a case stud...