Understanding Grand Minima in Solar Activity: Confronting Observations with Dynamo Simulations

TL;DR

This paper reviews recent research on solar grand minima, exploring observational, reconstructive, and simulation approaches to understand the mechanisms behind these extended periods of low solar activity.

Contribution

It synthesizes current understanding of solar grand minima and identifies key challenges requiring further investigation in solar physics.

Findings

Summarizes observational and simulation studies of grand minima

Highlights unresolved questions about solar magnetic activity transitions

Emphasizes need for integrated observational and modeling efforts

Abstract

The grand minimum in the Sun's activity is a distinctive mode characterized by a magnetic lull that almost completely lacks the emergence of sunspots on the solar surface for an extended duration. The factors driving this transition of an otherwise magnetically active star into a quiescent phase, the processes occurring within the solar interior and across the heliosphere during this period, and the mechanisms leading to the eventual resurgence of surface magnetic activity remain enigmatic. However, there have been sustained efforts in the past few decades to unravel these mysteries by employing a combination of observation, reconstruction and simulation of solar magnetic variability. Here, we summarize recent research on the solar grand minimum and highlight some outstanding challenges - both intellectual and practical - that necessitate further investigations.