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The solar mean magnetic field (SMMF) is referred to as the disc-averagedline-of-sight (LOS) magnetic field that also reflects the polarity imbalance ofthe magnetic field on the Sun. The origin of the SMMF has been debated over thepast few decades, with one school of thought suggesting that the contributionto the SMMF is mostly due to the large scale magnetic field structure, alsotermed as the background magnetic field, whereas other and more recent studieshave indicated that active regions have a major contribution to the observedSMMF. In this paper, we re-investigate the issue of the origin of the SMMF bydecomposing the solar disk into plages, networks, sunspots and backgroundregions, thereby calculating the variation in the observed SMMF due to each ofthese features. We have used full disk images from SDO/{\it AIA} recorded at1600~\AA\, for earmarking plages, networks and background regions and4500~\AA\, images for separating the sunspots. The LOS fields corresponding toeach of these regions are estimated from the co-temporal SDO/{\it HMI} fulldisk magnetograms. The temporal variation of the SMMF shows a near one-to-onecorrespondence with that of the background field regions suggesting that theyconstitute the major component of the observed SMMF. A linear regressionanalysis based on the coefficient of determination shows that the backgroundfield dominates, and accounts for 89\% of the variation in the SMMF whereas themagnetic field from the other features accounts for the rest 11\%.

On the variability of the solar mean magnetic field: contributions from various magnetic features on the surface of the Sun