Research

Research Interests

My research focuses on understanding the dynamic Sun through the lens of high-resolution observations, spectropolarimetry, and advanced data analysis.

A central theme in my recent work is the investigation of small-scale magnetic reconnection in the solar lower atmosphere — particularly phenomena like Ellerman bombs, which are increasingly recognised as key contributors to chromospheric heating and energy transport. I have shown that these events are not confined to active regions but are ubiquitous across the quiet Sun, often hidden in subtle signatures that require careful observation and analysis.

I am deeply involved in spectropolarimetric diagnostics to probe the solar magnetic field in both the photosphere and the chromosphere. My studies of sunspot penumbrae, quiet-sun regions, and transient events provide insights into the complex magnetic topology and its role in structuring the solar atmosphere.

Another aspect of my research explores chromospheric dynamics, such as spicules and small-scale downflows, which are vital to understanding the mass and energy balance between different layers of the Sun’s atmosphere.

In recent years, I have begun integrating machine learning techniques into solar physics to manage and interpret large volumes of data. This has proven particularly effective in identifying rare or weak events and patterns in spectral diagnostics.

My work combines ground-based and space-borne data with state-of-the-art radiative transfer modelling.

Research Highlights

Uncovering Ubiquitous Magnetic Reconnection in the Quiet Sun

One of the key highlights of my research is the detailed characterisation of quiet-Sun Ellerman bombs — small-scale magnetic reconnection events occurring in the lower solar atmosphere. Traditionally thought to be limited to active regions, my work has shown that these transient events are ubiquitous even in the quiet Sun, with potentially hundreds of thousands present at any given time. I have investigated their morphological, magnetic, and dynamic properties using high-resolution Hβ observations from the Swedish 1-m Solar Telescope, combined with spectropolarimetry and data-driven techniques such as machine learning. These findings extend our understanding of magnetic reconnection at the smallest observable scales and point to their potential role in heating the chromosphere and contributing to the mass and energy transport in the solar atmosphere.

How Sunspot Magnetic Fields Change During Waves and Flashes

The Sun’s atmosphere is constantly in motion — filled with waves and oscillations that travel through its different layers. These waves can become intense in sunspots, leading to dramatic brightenings known as umbral flashes and outward-moving patterns called running penumbral waves.

In this study, we investigated how these dynamic events affect the magnetic field in the chromosphere of sunspots. Using high-resolution observations in the Ca II 8542 Å line, we found that the magnetic field appears to strengthen during these events by a few hundred Gauss.

Our findings show that these changes are not just due to how we observe the Sun’s atmosphere but likely represent real variations in the magnetic field.

Detecting Overturning Convection in Sunspot Penumbrae

High-resolution observations using the 1-meter Swedish Solar Telescope revealed clear signatures of overturning convection in sunspot penumbrae. By analysing the deep-forming C I 5380 Å spectral line, strong redshifts were detected at the edges of bright penumbral filaments, consistent with downflows. In contrast, concentrated blueshifts at the filament heads indicated upflows. These flow patterns support magneto-convective models where hot plasma rises along filament cores and cooler plasma sinks along their edges. The results highlight the importance of accessing deep photospheric layers to understand energy transport processes within sunspot structures.

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