1. Basic Concepts 2. Sun and Heliosphere at Times of Solar Activity Minimum 2.1. Typical Solar Wind and its Sources 2.2. The Ballerina Model 2.3. Solar Wind Stream Structure 2.4. The Two Basic States of the Solar Wind 2.4.1. Differences 2.4.2. Communities 2.5. Solar Wind Acceleration and Expansion 2.6. Solar Wind Streams and Their Interactions 2.6.1. Corotating Interaction Regions in the Inner ...

Pickup ions, created by ionization of slow moving atoms and molecules well inside the heliosphere, provide us with a new tool to probe remote regions in and beyond the heliosphere and to study injection and acceleration processes in the solar wind. Comprehensive and continuous measurements of H, He, C, N, O, Ne and other pickup ions, especially with the Solar Wind Ion Composition Spectrometer (...

One of the fimdamental potential hazards to the “Fire” mission (Solar Probe) is the energetic particle environment near the sun. Heras et al., (1995), Sanahuja el al. (1995), and Sanahuja and Lario (1995) have modeled shock acceleration of low energy particles (< 2 MeV) due to fast ejects from the sun, One c@ical problem in this model, at the present time, is that no one has modeled coronal and...

The purpose of this study is to examine the spatial distribution of pick-up ions in a region with a macroscopic velocity shear, as may occur in the interaction of the solar wind with non-magnetic planets and comets. We calculate trajectories of individual contaminant particles for different orientations of the magnetic field. Density profiles are derived analytically for the case in which the s...

We present a four-category classification algorithm for the solar wind, based on Gaussian Process. The four categories are the ones previously adopted in Xu and Borovsky [2015]: ejecta, coronal hole origin plasma, streamer belt origin plasma, and sector reversal origin plasma. The algorithm is trained and tested on a labeled portion of the OMNI dataset. It uses seven inputs: the solar wind spee...

This paper presents the statistical analysis of the diurnal variations of the F layer at the equatorial station of Ouagadougou (Lat: 12.4 N; Long: 358.5 E; dip: 5.9 ) from 1966 to 1998 (=> ~11 680 days). We consider three main factors of variability: (1) the season (spring, summer, autumn and winter), (2) the phase of the sunspot cycle (ascending, maximum, descending and minimum) and (3) the ge...

This paper inspects possible influence of solar cycles on earthquakes through of statistical analyses. We also discussed the mechanism that would drive the occurrence of increasing of earthquakes during solar maxima. The study was based on worldwide earthquakes events during approximately four hundred years (16002010).The increase of earthquakes events followed the Maxima of Solar cycle, and al...

[1] Several observational studies suggest that solar wind dynamic pressure fluctuations can drive magnetospheric ultralow‐frequency (ULF) waves on the dayside. To investigate this causal relationship, we present results from Lyon‐Fedder‐Mobarry (LFM) global, three‐dimensional magnetohydrodynamic (MHD) simulations of the solar wind–magnetosphere interaction. These simulations are driven with syn...