In doing so, they’ve managed to solve an longstanding stellar mystery: why, as the solar wind travels away from the sun, does it quickly devolve from a structured series of rays into a gusty, turbulent mess? The answer lies in the magnetic field lines along which the solar wind travels.


It turns out the Sun’s magnetic control over the solar wind dissipates quickly as it exits the corona, dropping much faster than the pressure of the material inside the plasma itself. Released from their magnetic confinement, sharply defined rays start to break up and fan out, creating something more akin to a misty spray.

“Eventually, the material starts to act more like a gas, and less like a magnetically structured plasma,” Craig DeForest, lead author of a new study published in the Astrophysical Journal said in a statement.


To capture the transition zone, which occurs some 20 million miles ahead of the edge of the corona, STEREO images were carefully processed to remove the background glare of the stars. Here’s what those images looked like before and after processing:

Aside from reminding us that we’re ants at the mercy of a blowtorch, why are scientists so interested in studying the Sun’s energetic outbursts? For one, by understanding when and why the Sun is active, we can develop better models for predicting space weather here on Earth, and hopefully prevent an apocalyptic solar storm from annihilating us all.

Also, the first reason. The Sun is one gnarly beast.

[The Astrophysical Journal via NASA]