Interplanetary scintillationIn astronomy, interplanetary scintillation refers to random fluctuations in the intensity of radio waves of celestial origin, on the timescale of a few seconds. It is analogous to the twinkling one sees looking at stars in the sky at night, but in the radio part of the electromagnetic spectrum rather than the visible one. Interplanetary scintillation is the result of radio waves traveling through fluctuations in the density of the electron and protons that make up the solar wind.
SubstormA substorm, sometimes referred to as a magnetospheric substorm or an auroral substorm, is a brief disturbance in the Earth's magnetosphere that causes energy to be released from the "tail" of the magnetosphere and injected into the high latitude ionosphere. Visually, a substorm is seen as a sudden brightening and increased movement of auroral arcs. Substorms were first described in qualitative terms by Kristian Birkeland which he called polar elementary storms. Sydney Chapman used the term substorm about 1960 which is now the standard term.
Indice KpL’indice Kp (Kp index ou Planetary K-index) est souvent utilisé pour déterminer la probabilité de voir les aurores polaires. C’est aussi l’un des indices les plus couramment utilisés pour indiquer la gravité des perturbations magnétiques mondiales dans l’espace proche de la Terre. L’indice Kp est une moyenne pondérée de plusieurs indices K à partir d’un réseau d’observatoires géomagnétiques. Il fut introduit par Julius Bartels en 1939 et est tirée du mot allemand Kennziffer.
Solar stormA solar storm is a disturbance on the Sun, which can emanate outward across the heliosphere, affecting the entire Solar System, including Earth and its magnetosphere, and is the cause of space weather in the short-term with long-term patterns comprising space climate. Solar storms include: Solar flare, a large explosion in the Sun's atmosphere caused by tangling, crossing or reorganizing of magnetic field lines Coronal mass ejection (CME), a massive burst of plasma from the Sun, sometimes associated with s
Solar phenomenaSolar phenomena are natural phenomena which occur within the atmosphere of the Sun. These phenomena take many forms, including solar wind, radio wave flux, solar flares, coronal mass ejections, coronal heating and sunspots. These phenomena are believed to be generated by a helical dynamo, located near the center of the Sun's mass, which generates strong magnetic fields, as well as a chaotic dynamo, located near the surface, which generates smaller magnetic field fluctuations.
