For decades, scientists have observed the Sun’s behavior primarily through its visible surface features—sunspots, solar flares, and coronal mass ejections that rhythmically wax and wane in approximately 11-year cycles. These cycles, marking the ebbs and flows of solar magnetic activity, significantly influence space weather and, consequently, technological systems on Earth, including satellites, power grids, and communications networks. However, a groundbreaking study led by researchers at the University of Birmingham has unveiled a deeper, more nuanced understanding of these cycles, revealing critical structural changes in the Sun’s interior that have progressively migrated closer to its visible surface over the last four solar cycles.
The research team capitalized on nearly 40 years of helioseismic observations gathered by the Birmingham Solar Oscillations Network (BiSON). Unlike traditional methods that track solar phenomena only on or above the surface, helioseismology probes the Sun’s interior by analyzing sound waves resonating within it. These acoustic oscillations, known as p-modes, fluctuate in frequency in response to the Sun’s magnetic environment. Through detailed analysis of these frequency variations over solar cycles 22 through 25, spanning from 1987 to 2025, the study illuminated subtle but significant changes in the Sun’s subsurface magnetic structure.
The pivotal finding indicates that the Sun’s magnetic activity—historically diffused across various layers of the solar interior—is becoming increasingly confined to a shallow stratum roughly within 1,000 kilometers beneath the surface. This “skin-deep” localization contrasts markedly with previous cycles where magnetic phenomena permeated more deeply into the Sun’s interior. Such confinement suggests a marked reorganization in how solar magnetic fields are generated, stored, and evolve, potentially marking a long-term shift in solar dynamics.
Professor Bill Chaplin, leading the study, articulated this phenomenon as the Sun’s “active biorhythm,” a complex cadence of magnetic rise and fall that shapes space weather. The helioseismic data reveals that the connection between internal solar oscillations and surface magnetic activity indicators has shifted since solar cycle 23, signaling an evolutionary change in the Sun’s internal processes. This disparity underscores the limits of surface observations alone in grappling with the full complexity of solar activity.
Delving into the methodology, the study segregated the solar oscillations into low-, mid-, and high-frequency bands. Each frequency band probes a different depth below the solar surface, allowing researchers to map structural and magnetic variations at discrete layers. By comparing these oscillatory signatures with traditional surface activity metrics, the team discerned that while the surface magnetic indicators might reflect a weakening in the latest cycle (cycle 25), helioseismic data, particularly from high-frequency oscillations, reveal a persistently strong magnetic intensity beneath the surface.
This nuanced discrepancy not only challenges current models of solar cycle strength assessment but also indicates a potential shift in the underlying physics of the solar dynamo—the internal mechanism powering magnetic field generation. Professor Sarbani Basu of Yale University, a co-author of the study, emphasized that the evolving relationship between internal oscillations and surface magnetism cannot be explained simply by weaker magnetic fields. Instead, it points towards complex structural reorganization in the Sun’s magnetic storage and transport mechanisms within its outer layers.
Understanding these internal dynamics is crucial, as the Sun’s magnetic cycle directly impacts space weather. Periods of high solar activity, or solar maxima, often unleash intense solar flares and energetic particle storms that can disrupt global positioning systems, satellite operations, and terrestrial electrical infrastructures. As the Sun’s magnetic phenomena become more confined near the surface, this could influence the timing, intensity, and characteristics of such space weather events in ways not fully anticipated today.
The long-term BiSON dataset was instrumental in making this discovery possible. Such an extended observational record spanning nearly four decades allowed the researchers to detect subtle, systematic trends that would have otherwise remained obscured by shorter-term variability. The current Cycle 25 appears to be a particularly telling case, exhibiting pronounced signatures of the newly observed confinement effect, thus offering a natural laboratory for further study.
Looking ahead, continuous monitoring of solar oscillations through the remainder of Cycle 25 and into the upcoming Cycle 26 stands as a pivotal undertaking. Confirming whether these structural changes signify a permanent transformation or a transient fluctuation will refine modeling efforts and enhance predictive capabilities for solar activity. Such predictions hold the promise of mitigating the impact of space weather on crucial technologies and infrastructure on Earth and in orbit.
Beyond their immediate relevance to heliophysics, these findings offer profound insights into stellar physics more broadly. The Sun serves as the primary astrophysical laboratory for understanding magnetic activity in stars, and discoveries of restructured magnetic layering may aid in interpreting similar processes observed in other stars. Asteroseismology—the study of stellar oscillations—is poised to benefit from this pioneering work by providing new frameworks for connecting internal stellar dynamics with surface phenomena.
As the scientific community digests these revelations, the message is clear: the Sun is not a static entity but a dynamic star whose internal processes evolve over decades. Our capacity to “listen” to the Sun’s acoustic symphony has reshaped our understanding, revealing a vibrant, changing interior landscape intimately linked to the magnetic forces sculpting space weather. This research highlights the importance of sustained, high-precision observations and sets the stage for the next generation of solar physics investigations.
In sum, the evolving confinement of solar magnetic activity near the surface challenges pre-existing paradigms and underscores the need for comprehensive, multi-layered approaches to unravel the complexity of our star’s behavior. With space weather increasingly entwined with our technological civilization’s fabric, deciphering the Sun’s internal transformations remains a compelling scientific frontier with tangible societal implications.
Subject of Research: Changes in solar interior structure and magnetic activity using helioseismology.
Article Title: Sub-surface structural changes associated with successive 11-yr solar activity cycles have been progressively more confined near the surface: new helioseismic results on Cycles 22–25 from BiSON
News Publication Date: 28-May-2026
References: Chaplin, W. J., et al. (2026). Sub-surface structural changes associated with successive 11-yr solar activity cycles have been progressively more confined near the surface: new helioseismic results on Cycles 22–25 from BiSON. Monthly Notices of the Royal Astronomical Society.
Image Credits: W. J. Chaplin
Keywords
Solar activity, solar cycles, helioseismology, stellar oscillations, solar interior, magnetic fields, space weather, Birmingham Solar Oscillations Network, BiSON, solar dynamics, asteroseismology, solar dynamo
Tags: Birmingham Solar Oscillations Networkhelioseismology solar researchlong-term solar observationsp-mode acoustic oscillationssolar cycle 22 to 25 analysissolar cycle magnetic shiftssolar magnetic activity evolutionsolar oscillation frequency variationsspace weather impact on technologysubsurface solar magnetic fieldssun interior structural changestechnological systems and solar weather
