Magnetic storm (Solar storms)
The Sun, characterized by its dynamic nature as a sphere of gas, undergoes continual activity in accordance with cyclical patterns referred to as the solar cycle. This activity, inclusive of phenomena like solar flares and coronal mass ejections (CMEs), plays a significant role in shaping the energy and velocity of the solar wind, as well as the potency of the interplanetary magnetic field (IMF).
Solar flares represent massive eruptions occurring on the Sun's surface, while CMEs manifest as substantial clouds of charged particles expelled from the Sun's corona along intense magnetic field lines over extended durations. Despite Earth's magnetic field deflecting a portion of the solar wind, some particles manage to breach this barrier, leading to magnetic disturbances termed geomagnetic storms or substorms. While geomagnetic storms can give rise to captivating auroras, they also pose risks as detrimental space weather occurrences.
Geomagnetic storms are classified into recurrent and non-recurrent categories. Recurrent storms, linked to the Sun's rotational cycle, recur every 27 days and are triggered by Earth's interaction with the southward IMF during the solar minimum phase. Non-recurrent storms, more prevalent during the solar maximum, arise from CMEs and their interaction with interplanetary shock waves.
Substorms, akin in origin to geomagnetic storms, are brief episodes lasting two to three hours and occur more frequently, up to six times daily, during the storm's developmental phase. While substorms are confined to auroral zones, magnetic storms impact the entire globe.
Solar activity adheres to cyclic patterns, with maximum sunspot conditions recurring approximately every 11 years. During these phases, sunspot groups undergo rapid expansion and rotation, triggering explosive energy releases known as solar flares. Despite the vast distance separating Earth from the Sun, Earth's systems exhibit synchronization with the solar cycle.