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The horizontal line shows the mean of peaks of the monthly BMRs obtained for last 13 observed solar cycles.
SOLAR FLARE 3D MODEL SERIES
However, when observed Gaussian scatter of BMR tilts around Joy’s law 3 with a standard deviation (σ δ) of 15° is considered, our model produces a variation in the solar cycle, including north-south asymmetry comparable to the observations (Figure 2b).įigure 2| Time series of the monthly sunspot number (which is same as the BMR number) from the simulation (a) without tilt scatter (Ref. The randomness and nonlinearity in the BMR emergences make the poloidal field unequal and cause some variability in the solar cycle (Figure 2a). We find that a little quenching in the BMR tilt, as shown in Figure 1, is sufficient to stabilize the dynamo growth. Note that the dashed line deviates from Joy’s law (solid line) due to the non- linear quenching introduced in it. The solid, dashed, and dotted lines respectively show the actual Joy’s law: δ = 35°sin λ, the mean BMR tilts in each latitudes, and the zero line. 1): BMR tilts versus latitudes (λ) shown only from the northern hemisphere data. In this updated model, based on the toroidal flux at the base of the convection zone, bipolar magnetic regions (BMRs) are produced with statistical properties obtained from observed distributions.įigure 1| Result from a dynamo simulation with Gaussian tilt scatter of σ δ = 15° around Joy’s law (Ref. This model is an updated version of the original model developed by M. We explore the cause of this solar cycle irregularities using a novel 3D kinematic Babcock–Leighton dynamo model. The extreme example of this irregularity is the Maunder minimum in the 17th century when sunspot cycle went to a very low value. The solar magnetic cycle is not regular, and the individual cycle strength and duration vary cycle-to-cycle. High Altitude Observatory, NCAR, Boulder, CO 80301, USA Indian Institute of Technology (BHU), Varanasi, IndiaĢ.