Read or download the official PDF of this gazette notification issued by the Ministry of Science and Technology on 13th August 2026. Classified under Press Release.
Executive Summary
A multi-institutional team led by the Indian Institute of Astrophysics (IIA) has developed a three-dimensional magnetohydrodynamic computer simulation model to forecast the arrival and impact of Coronal Mass Ejections (CMEs). Published in the Astrophysical Journal, the study establishes that the rate of magnetic reconnection directly correlates with CME acceleration, offering a new tool to predict these powerful solar events. This research aims to mitigate potential damage to satellite systems, power grids, and global communications by improving early warning capabilities.
Key Points / Main Content
Technological Development
3D MHD Model: Scientists developed a sophisticated three-dimensional magnetohydrodynamic (MHD) simulation model to trace the step-by-step evolution of magnetic energy.
NOVA HPC Facility: The computational work was performed using the high-performance computing infrastructure at the IIA data center.
Dual Approach: The study combined computer simulations of successive flux rope eruptions with cross-validation using observational data from NASA’s Helioseismic and Magnetic Imager (HMI) and Atmospheric Imaging Assembly (AIA).
Mechanism of CMEs
Magnetic Flux Ropes (MFRs): The model identifies MFRs—twisted bundles of magnetic field lines—as the primary triggers of CMEs.
Reconnection Process: The simulation shows how magnetic field lines snap and reconnect at a "current sheet," releasing the energy required to launch a CME.
Gradual Initiation: Eruptions do not begin explosively; they start with the slow formation of a thin electric current sheet that intensifies over time, leading to a large-scale expulsion.
Scientific Findings
Acceleration Correlation: A striking result of the study is that the rate of magnetic reconnection correlates with CME acceleration in a clear, monotonic fashion.
Predictive Factor: Reconnection flux is identified as the critical factor in determining how fast and how energetically a CME will erupt.
Impact Analysis
Solar Physicists and Scientific ResearchersImpact
Researchers now have a clearer understanding of the "mystery" regarding how magnetic energy builds up and is released. The model provides a framework to study the chain of events transforming solar magnetic structures into violent explosions.
Action Required
Scientists should utilize the model’s findings to refine solar weather forecasting and further explore the relationship between reconnection rates and eruption intensity.
Global Communications and Infrastructure ProvidersImpact
Improved forecasting of CMEs can help protect critical infrastructure, including satellite systems, power grids, and global communication networks, from the damaging effects of magnetized plasma.
Action Required
Stakeholders in these sectors should monitor the integration of this simulation model into space weather warning systems to improve disaster preparedness and mitigation strategies.
International Research Institutions (IIA, DST, University of Helsinki, NASA)Impact
The successful multi-institutional collaboration demonstrates the effectiveness of combining international observational data with domestic high-performance computing.
Action Required
Participating institutions should continue to support collaborative cross-validation efforts between simulation models and real-time observational instruments.
Key Entities Referenced
Indian Institute of Astrophysics (IIA): The lead research organization under the Department of Science & Technology that developed the 3D computer simulation model to forecast Coronal Mass Ejections (CMEs).
Department of Science & Technology (DST): The primary government department overseeing the autonomous research initiative and the development of solar event forecasting models.
Astrophysical Journal: The peer-reviewed scientific publication where the research findings regarding magnetic flux rope eruptions and model validation were published.
NOVA HPC facility: The high-performance computing infrastructure hosted at the IIA data center used to execute the complex 3D magnetohydrodynamic (MHD) simulations.
NASA: The agency that provided critical observational data through the Helioseismic and Magnetic Imager (HMI) and Atmospheric Imaging Assembly (AIA) for model cross-validation.
Ministry of Science & Technology
New computer model can help trace magnetic
energy builds up & forecast impact of resulting
CMEs
प्रव तथ: 13 AUG 2026 5:02PM by PIB Delhi
A multi-institutional team of scientists have developed a three-dimensional computer simulation model
that can bring scientists a step closer to forecasting the arrival and impact of Coronal Mass Ejections
(CMEs) before they reach Earth.
CMEs are among the most dramatic and powerful events in our solar system — gigantic eruptions of
magnetized plasma hurled from the Sun at millions of kilometres per hour. When directed toward Earth,
they can damage satellite systems, disrupt power grids, and interfere with global communications. At the
heart of these eruptions lie magnetic flux ropes (MFRs), which are twisted bundles of magnetic field lines
embedded in the plasma, and are widely regarded as the primary triggers of CMEs. Yet, how the magnetic
energy builds up, and is then released during CMEs has remained one of solar physics' most stubborn
mysteries through the violent expulsion has been poorly understood until now.
Fig 1: Snapshots from our simulation showing a twisted magnetic structure — called a flux rope — rising
through the Sun's outer atmosphere. The red threads represent the Sun's background magnetic field, while
blue, green, and cyan threads trace the emerging rope from its core outward. The full animation covers
about 20 hours of solar time and ends with the rope being violently ejected into space.
In order to trace the evolution of the magnetic energy to CMEs researchers at the Indian Institute of
Astrophysics, an autonomous institute of the Department of Science & Technology (DST), Govt. of India,
along with their collaborators, have developed sophisticated three-dimensional magnetohydrodynamic(MHD) computer simulation model.
This model traces, step by step, how the reconnection flux changes as a magnetic flux rope rises, stretches
the surrounding ambient magnetic field, and ultimately erupts. The model begins with a realistic coronal
setup of a solar atmosphere, which is threaded by a magnetic field configuration resembling a coronal
streamer in observation. A twisted magnetic flux rope is gradually introduced into this from below,
mimicking how new magnetic flux emerges from beneath the solar surface.
Fig 2: The reconnection engine, caught in the act. The white surface (panel a) marks the current sheet —
where the Sun's magnetic field lines snap and reconnect, releasing the energy that launches a CME. The
S-shaped field lines in panels (b) and (c) are the magnetic threads passing through this energy release site.
The computational work in this study was performed on the NOVA HPC facility. This high-performance
computing infrastructure is hosted at the data center of the IIA.
As the flux rope rises, the team observed in their computer models that the overlying magnetic field is
significantly stretched and compressed beneath it. Reconnection does not begin explosively. Instead, it
starts quietly with the slow formation of a thin sheet of strong electric current, a thin layer where opposing
magnetic fields are pushed together. Over time, this process intensifies, culminating in the impulsive,
large-scale expulsion of the flux rope.
What makes this study published in Astrophysical Journal particularly compelling is its dual approach.
The researchers not only simulated two successive flux rope eruptions in their model, but also cross-
validated their findings with another researcher from the University of Helsinki, Finland, who teamed up
with the Indian group to contribute analysis based on observational data from NASA's Helioseismic and
Magnetic Imager (HMI) and the Atmospheric Imaging Assembly (AIA), two of the most powerful
instruments currently observing the Sun.Fig 3: Seeing reconnection from Earth. Left: the flash of the flare. Right: its magnetic footprint — color-
coded ribbons sweeping outward across the Sun's surface over 36 minutes. The area swept by these
ribbons is our observational measure of how much magnetic flux was reconnected during the eruption.
The comparison between simulation and observation revealed a striking result: the rate of magnetic
reconnection correlates the acceleration of the CME in a clear, monotonic fashion, meaning that as
reconnection speeds up, so does the eruption, from start to finish. This finding establishes reconnection
flux as a critical factor in determining not just whether a CME erupts, but how fast and how energetically
it does so.
This work by the team comprising Dr. Samriddhi Sankar Maity (Postdoc at NASA & Georgia State
University, USA), Dr. Piyali Chatterjee, IIA and Mr. Ijas S Mytheen (PhD student, Eotvos University,
Hungary) and Dr. Ranadeep Sarkar from the University of Helsinki, Finland, offers important new insight
into the chain of events that transforms a slowly building magnetic structure into one of the powerful
explosions in our solar system.
Publication link: https://iopscience.iop.org/article/10.3847/1538-4357/ae3d9a.
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