Both sunspot numbers (SSN) and the heliospheric magnetic field (HMF) show approximately 11-year cycles that superpose longer-term quasi-periodic variations, called secular variations (for more information on solar cycles refer to Hathaway, 2010). Some of the more prominent secular variations are three grand minima: the Wolf (years 1280-1350), Maunder (years 1645-1710), and Dalton minima (years 1790-1830, solar cycles 6-8). In addition, the space age has coincided with the longest grand maximum in 9300 years (Abreu et al., 2008). But the duration of previous maxima and the quasi-periodic recurrence of these secular variations suggests that this grand maximum is ending, and the Sun is entering a possible grand minimum-a modern minimum.While the 11-year solar cycles have been known for over a century, the physics behind it is not fully agreed-upon (Charbonneau, 2010). Variations of the solar magnetic field can be qualitatively described based on the oscillatory exchange of energy between poloidal and toroidal solar magnetic field components as a driving force for solar cycles. In this model, the toroidal magnetic field is generated by buoyant upwelling within the convective zone, which is itself created by the differential rotation of the Sun stretching the large-scale poloidal component and appears as bipolar magnetic regions (BMRs) on the Sun's surface. The effect of Coriolis force on the rising toroidal magnetic flux tubes tilts these BMRs, and turbulent convection further leads to a dispersion around the mean tilt. The poloidal component of the solar magnetic field and the resulting active regions reach their maximum during solar maximum. A poloidal dipolar field, on the other hand, is created by the shift of energy from the toroidal field to the poloidal field due to the dispersion and decay of the BMRs via surface flux transport processes during the declining phase of the solar cycle (Babcock, 1961;Bhowmik & Nandy, 2018;Leighton, 1969). The largescale solar magnetic field that is tied to the solar activity cycles as described above governs the coronal conditions and plays a role in balancing the heliospheric open flux and the resulting HMF (see e.g., Pal et al., 2020;Schwadron et al., 2010).Many attempts have been made to understand the cause of the longer-term solar variations. These variations dictate the amplitude of the solar cycles (