Abstract Temporal variations in the number and area of coronal bright points (CBPs) were studied separately in the northern and southern hemispheres over more than two solar cycles (years 1996–2022). Hemispheric asymmetry was identified in both the total number and area of CBPs, with differences reaching up to 15percnt. Statistical analysis using Student’s t-test confirms that these differences are statistically significant. The observed asymmetry arises from the asynchronous formation of CBPs in the hemispheres, rather than from the asymmetry of active regions. These variations in asymmetry are explained by the existence of two different types of CBP: ‘bright’ and ‘dim’. Differences in the asymmetry and overall number variations between these two types during solar cycles suggest distinct physical mechanisms underlying their formation. Bright CBPs closely follow the patterns of active regions, supporting the hypothesis that they are miniature active regions formed through similar mechanisms. In contrast, dim CBPs, predominantly located in quiet Sun regions, often display behavior opposite to sunspots, partially attributable to the visibility effect and influence of active regions. However, the temporal variations in the normalized asymmetry index indicate that visibility effect alone cannot fully explain the observed patterns. The relatively uniform asymmetry of dim CBPs across 11-year solar cycles supports the hypothesis of a cycle-independent (or dependent on a longer period) component of the solar dynamo, potentially linked to a small-scale turbulent dynamo.
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