Solar system: Interplanetary kidnap

Solar Wind Anr Interplanetary Magnetic Field

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 ...

Interplanetary Field Visualization System

A prototype system of visualizing interplanetary field has been developed using an immersive projection display. The system enables a user to observe global behavior of the interplanetary plasma in a virtual environment. The velocity and density fluctuations are measured with interplanetary scintillation method, and are analyzed by using computer topography technique. The analysis has produced ...

Tomography of the Solar Wind using Interplanetary Scintillation

Interplanetary Lyman α line profiles : variations with solar activity cycle

Aims. Interplanetary Lyman α line profiles are derived from the SWAN H cell data measurements. The measurements cover a 6-year period from solar minimum (1996) to after the solar maximum of 2001. This allows us to study the variations of the line profiles with solar activity. Methods. These line profiles were used to derive line shifts and line widths in the interplanetary medium for various an...

Solar Wind and Interplanetary Magnetic Field: A Tutorial

The convection layer completes the transport of energy from the nuclear furnace at the center of the sun to its radiation into space by the photosphere, but most importantly for the solar wind it sets the temporal and spatial scales for the structure of the coronal magnetic field that in turn controls the properties of the solar wind. In this tutorial review we examine the properties of the fie...