This post was originally published on here
The Sun looks simple when you’re not thinking too hard about it. A bright yellowish-white disk in the sky. A reliable source of warmth. Something you don’t stare at unless you enjoy retinal damage. But when scientists break its light down into a spectrum, the idea of a simple Sun falls apart.
Spread sunlight into a rainbow, and you don’t get a smooth gradient. You get thousands of thin dark gaps where certain colors are missing. These gaps are known as Fraunhofer lines, first cataloged in 1814 by German physicist Josef von Fraunhofer. Most of them make sense. Specific atoms and molecules in the Sun’s atmosphere absorb light at specific wavelengths, leaving behind dark fingerprints in the spectrum. That’s how scientists know the Sun contains hydrogen and helium, along with oxygen, sodium, calcium, iron, and trace amounts of heavier elements.
Videos by VICE
The problem is that not all of those missing colors correspond to any known element or molecule.
Researchers can see these missing colors clearly when they observe the Sun directly. The trouble starts when they try to reproduce them. Models built from everything we know about the Sun simply don’t generate the same missing features.
That’s certainly not because researchers haven’t tried. According to a 2017 study, one major issue is that our databases of atomic and molecular spectral lines are incomplete. Some elements, especially those in the iron group, produce incredibly complex absorption patterns that are difficult to measure and verify in the lab. Others may involve molecules that don’t behave cleanly under solar conditions.
Then there’s the Sun itself. Its atmosphere isn’t calm or uniform. At all. Hot plasma rises and falls through convection. Magnetic fields twist, snap, and interfere with how light escapes. These conditions can distort absorption features in ways that simplified models struggle to reproduce.
The implications extend well past the Sun. When the universe first formed, it was mostly hydrogen and helium. Heavier elements only appeared later, forged inside stars and scattered when those stars died. By reading a star’s spectrum, scientists can estimate its age and history. The Sun, as our closest star, should be the easiest case. The fact that it still produces unexplained signals highlights how tricky stellar physics really is.
The mystery lines aren’t a failure, though. They’re clues. Each mismatch between observed sunlight and modeled spectra points to gaps in our understanding, whether that’s missing atomic data or oversimplified assumptions about solar behavior.
The Sun is the most studied star we have, and parts of its light still don’t have a solid explanation.
