This article has been reviewed according to Science X's editorial process and policies. Editors have highlighted the following attributes while ensuring the content's credibility: In a new study, a team of astronomers has identified wavelengths of light that could be useful for tracing the chemical evolution of the universe. Using computational modeling to simulate how electrons interact with manganese ions—an element produced during stellar explosions called supernovae—researchers predicted how different environmental conditions could produce observable light known as emission lines.
They found that certain emission lines were extremely sensitive to changes in the temperature and density of the surrounding nebula, meaning they could be useful tools for analyzing rapidly expanding objects like supernova remnants and other large gas clouds, said Anil Pradhan, a professor of astronomy at The Ohio State University and co-author of the study published in Monthly Notices of the Royal Astronomical Society. "If we understand the chemical composition of galaxies, we can learn more about the chemistry of stars and their elements," said Pradhan. "That will eventually lead to understanding the evolution of the universe and the composition of everything within it." Stellar explosions play a crucial role in the formation of heavy elements like iron and other metals, which are essential to the evolution of stars, planets and other cosmic objects.
Manganese is a key element because its abundance increases over time, meaning researchers can use it as a cosmological clock to learn more about how galaxies evolve. "Space and time are related, so measuring manganese abundances can grant us insight into the ever-expanding nature of the universe," said Pradhan. "By combining this emission line data with other known facts on important elements like oxygen and sulfur, we may be able to view some of the earliest observable epochs in the history of the universe." Still, depending on their strength, faint emission lines can be extremely difficult and time-consuming to detect.
To overcome these limitations, Pradhan and his colleagues employed powerful computing systems to model the behavior of more than 700 potential emission lines using atomic physics calculations that would otherwise have taken years to complete. Though their work is still theoretical, the findings suggest that once paired with real-world astronomical observations, these conclusions could be used to predict the conditions of other types of complex space environments, said Pradhan. Moreover, understanding manganese's role in the cosmos could help scientists predict the universe's chemical future.
"We're getting better and better at capturing energy that reveals the shape of the universe," said Pradhan. "This work joins astrophysics, atomic physics and plasma physics, and we're on the cusp of discovering many new processes." The team plans to verify their data using the James Webb Space Telescope and other ground-based observatories that specialize in detecting chemical variations across time and space. The results from this work will also be made publicly available so researchers can compare their data sets with novel atomic analyses, laying the foundation for similar chemical discoveries.
Zher Samak et al, Emissivity line ratios for [Mn ⅠⅠⅠ ] and spectral diagnostics of H ⅠⅠ regions, Monthly Notices of the Royal Astronomical Society (2026). DOI: 10.1093/mnras/stag1304 Journal information: Monthly Notices of the Royal Astronomical Society BA art history, MA material culture. Former museum editor, paramedic, and transplant coordinator.
Extract — continue reading at the source.
