Three-dimensional exploration of the solar wind using observations of interplanetary scintillation

Interplanetary scintillation observations of interaction regions in the solar wind

Co-rotating interaction regions (CIRs) between fast and slow streams of plasma are a prominent feature of the solar wind. Measurements of interplanetary scintillation (IPS) using the three widely separated antennas of the EISCAT facility have been used to detect the compression regions at the leading edges of interaction regions and to determine the location and velocity of the structure. Obser...

Tracking heliospheric disturbances by interplanetary scintillation

Coronal mass ejections are known as a solar cause of significant geospace disturbances, and a fuller elucidation of their physical properties and propagation dynamics is needed for space weather predictions. The scintillation of cosmic radio sources caused by turbulence in the solar wind (interplanetary scintillation; IPS) serves as an effective ground-based method for monitoring disturbances i...

Developments in the use of EISCAT for interplanetary scintillation

The antennas of EISCAT have been used for interplanetary scintillation (IPS) studies of the solar wind for many years. The main science found from these studies is obtained through the cross-correlation of signals from antennas having the longest baseline, providing more accurate information on the different solar wind streams which may be present in the line of sight. The development of dualfr...

EISCAT measurements of the solar wind

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...

Tomography of the Solar Wind using Interplanetary Scintillation