The Sun’s Colossal Glowing Loops, Up Close and Personal

By Tom Yulsman | December 12, 2014 1:40 pm

This visualization shows magnetic field loops in a portion of the Sun. The colors depict the strength of magnetic fields, with blue representing the weakest fields and red the strongest. The simulation was run on the Pleiades supercomputer at the NASA Advanced Supercomputing facility at NASA’s Ames Research Center in California. (Source: Robert Stein, Michigan State University; Timothy Sandstrom, NASA/Ames)

The gargantuan glowing loops that quiver and dance at the Sun’s surface are absolutely mesmerizing. If you’ve never seen them up close and personal, make sure to check out the videos a little lower down in this post.

But first, have a look at the image above. It is a supercomputer visualization that allows us to see what it would be like to fly through them.

To understand what you’re looking at, you first need to understand how these features form. First, consider the Sun’s prodigious energy created by the furnace at its core. Those nuclear fusion fires burn at an unimaginably hot 27 million degrees F. This is so rip-roaring intense that it tears atoms asunder, creating a roiling soup of charged particles called a plasma.

As is the case with all charged particles, magnetic fields are generated when they move about. And the Sun’s plasma moves around and interacts a whole lot.

Here’s the result, as explained by a primer at NASA’s Marshall Space Flight Center:

Magnetic field lines loop through the solar atmosphere and interior to form a complicated web of magnetic structures. Many of these structures are visible in the chromosphere and corona, the outermost layers of the Sun’s atmosphere.

As the lines of magnetic force emerge from beneath the Sun’s surface, they heat the corona and lead to sunspots, gigantic explosions of radiation called solar flares, and coronal loops. Visualizations produced by supercomputer simulations, like the one at the top of this post, help scientists understand these processes. In that image, the colors depict the strength of the magnetic field, with blue representing the weakest fields and red the strongest.

And here is the real thing — a movie acquired in the extreme ultraviolet portion of the spectrum by NASA’s Solar Dynamics Observatory. It covers a period of about 50 hours on Oct. 28, 2014.

As the Sun rotates, an active region crackles and pops with solar flares. And check out those loops. They glow as hot plasma flows along the gracefully curving magnetic field lines.

Here’s another video showing loops emerging from an active region on the Sun between December 7th and 9th, 2014:

This video is at lower resolution that the one above. But I still find it mesmerizing. And check out the little insert showing the Earth at lower left. That’ll give you a sense of the astounding scale of these features.

For more about the Sun’s coronal loops, go here.

CATEGORIZED UNDER: Physics, select, Solar System, Sun, Top Posts


ImaGeo is a visual blog focusing on the intersection of imagery, imagination and Earth. It focuses on spectacular visuals related to the science of our planet, with an emphasis (although not an exclusive one) on the unfolding Anthropocene Epoch.

About Tom Yulsman

Tom Yulsman is Director of the Center for Environmental Journalism and a Professor of Journalism at the University of Colorado, Boulder. He also continues to work as a science and environmental journalist with more than 30 years of experience producing content for major publications. His work has appeared in the New York Times, Washington Post, Audubon, Climate Central, Columbia Journalism Review, Discover, Nieman Reports, and many other publications. He has held a variety of editorial positions over the years, including a stint as editor-in-chief of Earth magazine. Yulsman has written one book: Origins: the Quest for Our Cosmic Roots, published by the Institute of Physics in 2003.


See More


Discover's Newsletter

Sign up to get the latest science news delivered weekly right to your inbox!

Collapse bottom bar