Interplanetary solar wind parameters (velocity of solar wind particle [Vp], proton density [Nsw], and component of solar magnetic field [IMF‐Bz]) and geomagnetic indices (symmetric horizontal component of geomagnetic field [SYM‐H], auroral electrojet [AE]) divulge great deal of information about geomagnetic disturbances. To better understand the influence of solar wind invasion into the energy dynamics of magnetosphere system, we have chosen five geomagnetic disturbance events of completely different nature as the quietest days, intense storm, High Intensity Long Duration Continuous Auroral Activity, Substorm, and Supersubstorm. The statistical analysis of these five events clearly supports the case that most of the time IMF‐Bz plays major role to create magnetic reconnection leading to the geomagnetic disturbances. Our study shows that Joule heating covers the largest fraction of energy dissipation, averaging 53.6% of total deposited energy for all events. Even though, in case of Supersubstorm, the major contribution due to the ring current (47%) surpasses Joule heating (43%). The cross‐correlation analysis applied for the IMF‐Bz with SYM‐H, solar wind energy and magnetospheric sinks explain and quantify the relation between them. The positive correlation of IMF‐Bz with SYM‐H value in each event delineates that southward orientation of IMF‐Bz is responsible for the depression of SYM‐H. However, an interesting result that IMF‐Bz correlated negatively with SYM‐H value for the quiet event suggests the southward orientation of IMF‐Bz does not necessarily have to be the cause of disturbance always. In few occasion, Solar Quiet (Sq) and Lunar (L) current is found to be taking over the role of IMF‐Bz to create disturbance.

This work presents the study of the quietest time variation in relativistic electrons, auroral precipitation, ring current, and joule heating during 1999, 2000, and 2004. Geostationary Operational Environmental Satellite (GOES) data on relativistic electrons with energies above 0.6 MeV, 2 MeV, and 4 MeV were analyzed. The time-series analysis of the relativistic electrons over a 24-hour averaged interval reveals a precise 24-hour modulation of the relativistic electron population during all seasons for energies above 0.6 MeV and 2 MeV, and during the winter season for higher energies above 4 MeV. In addition, relativistic electron fluxes at energies above 0.6 MeV and above 2 MeV were higher during the descending phase of the solar cycle compared to the ascending and solar-maximum phases. The cross-correlation analysis presented a strong correlation of Joule heating, ring current, and auroral precipitation with the relativistic electron population in three energy bands considered, as indicated by the zero-time lag. Studying the quiet time variation of relativistic electrons will lead to more complete ionospheric models, which were previously limited to the geomagnetically disturbed period.

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