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Geomagnetic storms (GMSs) are stimulated by higher solar wind flow speed (VSW) and by a southward-directed interplanetary magnetic field (IMF Bz). Two kinds of flows dominate the large scale structure of solar wind: corotating flows and transient disturbances. Corotating flows are associated with spatial variability in coronal expansion and solar rotation, whereas transient disturbances are associated with episodic ejections of material into interplanetary space from coronal regions. The high speed streams originated from coronal interaction regions (CIRs) and transient disturbances are mostly caused by fast coronal mass ejections (CMEs). CMEs are the crucial link between solar activity and transient interplanetary disturbances and are responsible for major GMSs. CMEs eject magnetic flux into interplanetary space that produces abrupt increase in the northward component of Earth's magnetic field. There are two types of geomagnetic field variations termed as long-time variation and storm-time variations. The long-term variations are very useful to solar cyclical study of geomagnetic field variation as well as change in polarity of the Sun, climate change, plants growth rate and geological change of Earth's pole. The storm time variations also known as geomagnetic storm deals the various characteristics of GMSs and their connection with solar source activities and interplanetary magnetic fields. These variations are directly affect us and shows adverse effect in satellites, communication system and power losses. In the present study, we have analysed large geomagnetic storms (GMSs) associated with storm time index (D st ) decrease of more than 100 nT observed during solar cycle 23

Study of large geomagnetic storms (GMSs) and their association with different solar source activities observed during solar cycle 23