Mark A. Carter

MAGNETARS should freak you out

World famous Canadian Science Fiction writer Mark A. Carter reprints an article from penned by Astrophysicist Paul Sutter from August 14, 2015 to give the reader a greater appreciation of the dynamics underlying Black Holes and there ilk. In this article, Dr. Sutter states: "In a magnetar's field, you just kind of dissolve." Now imagine Joe Cooper falling into the black hole named Gargantua in Christopher Nolan's film Interstellar, and tell me if you believe it. Right. Sure. You bet.

This artist's impression shows a magnetar in the very rich and young star cluster Westerlund 1.

Image is courtesy of Wikipedia: the free encyclopedia.

This cluster contains hundreds of very massive stars, some shining with a brilliance of almost one million suns. European astronomers have for the first time demonstrated that this magnetar, an unusual type of neutron star with an extremely strong magnetic field, probably was formed as part of a binary star system. The discovery of the magnetar's former companion elsewhere in the cluster helps solve the mystery of how a star that started off so massive could become a magnetar rather than collapse into a black hole.

I'll be honest: Magnetars freak me out. But to get to the why, I have to explain the what. Magnetars are a special kind of neutron star, and neutron stars are a special kind of dead star.

They're easy enough to make if you're a massive star. All stars fuse hydrogen into helium deep in their cores. The energy released supports the stars against the crushing weight of their own gravity and, as a handy by-product, provides the warmth and light necessary for life on any orbiting planets. But eventually, that fuel in the core runs out, allowing gravity to temporarily win and crush the star's core even tighter.

With the greater pressure, it becomes helium's turn to fuse, combining into oxygen and carbon, until the helium, too, gives out. That's where our own sun gets off the fusion train, but more massive stars can keep on chugging along, climbing up the periodic table in ever more intense and short-lived reaction phases, all the way up to nickel and iron.

Once that solid lump of nickel and iron forms in the stellar core, a lot of things go haywire fast. There's still a lot of star stuff left in the atmosphere, pressing into that core, but further fusion doesn't release energy, so there's nothing left to prevent collapse.

And collapse it does: The nickel and iron nuclei (yes, just nuclei; don't even think about entire atoms at these temperatures and pressures) break apart. They just can't handle this nuclear mosh pit. Stray electrons get shoved into the nearest protons, converting them to neutrons. The neutrons stay neutrons. And those neutrons are mighty good at preventing further collapse, for reasons I'll explain in a bit. The infalling gas, trying to crush the core into oblivion, bounces off that neutron core and goes kablamo! (Note: I don't know what it actually sounds like.)

The neutron ball:
What happens during the supernova event is an exciting discussion for another day. What we're concerned with now is the leftovers: a soupy, ball-like mixture of neutrons and a few straggler protons. This ball is supported against its own weight by degeneracy pressure, which is a fancy way of saying that you can only pack so many neutrons in box or, in this case, a ball. It may seem obvious that neutrons, well, take up space, but things didn't have to turn out this way. It's this degeneracy pressure that causes the big bounce that puts the super in supernova.

I should note that, if there's still too much stuff left hanging out around this leftover neutron ball, the weight can overwhelm even degeneracy pressure. And now, look what you've done: You've gone and made a black hole. But that, too, is another story. We wouldn't want to be like our poor star and get overwhelmed.

The neutron ball, which I should now call by its proper name: a neutron star, is weird. Seriously, that's the best word I can find to describe it. Neutron stars are basically city-size atomic nuclei, which makes them among the densest things in the universe. The pressure of gravity inside these stars has squeezed apart even atomic nuclei, allowing their bits to float freely.

It's mostly neutrons down there, hence the name, but there are also a few surviving protons floating around. Normally, those protons would repel one another, being like-minded charges and all, but they are forced close together as the Strong Nuclear Force tries to bunch them up with their fellow neutrons.

The neutron star's interior is a complicated dance of physics under extreme conditions, resulting in very odd structures. The oddity starts near the surface, with blobs of a few hundred neutrons that are best described as neutron gnocchi. Below that, the neutron blobs glue together into long chains. We have entered the spaghetti layer. Underneath that, at even more extreme pressures, the spaghetti strands fuse side by side and form lasagna sheets. Under it all, even neutron lasagna loses its shape, becoming a uniform mass. But that mass has gaps in it, in the form of long tubes. At last: delicious penne.

I wish I was making these names up, but physicists must be especially hungry people when coming up with metaphors.

Did I mention the spinning? Oh yes, neutron stars spin, up to a few hundred times per second. Let all of this sink in for a bit. An object with such strong gravity that hills are barely a few millimeters tall, rotating with a speed that could rival your kitchen blender. We're not playing games anymore.

Neutron stars are scary:
All this action: the insane densities, the complicated structures, and the ridiculously fast rotation rates, means that neutron stars carry some pretty nasty magnetic fields. But don't magnetic fields require charged particles, and aren't neutrons neutral? That's true, smarty pants, but there are still a few protons hanging out in the star, and at these incredible densities, physics gets complicated. So, yes: neutron stars, despite their name, can carry magnetic fields.

How strong are they? Take a star's normal magnetic field, and squish it down. Every time you squish, you get a stronger field, just as you get higher densities. And we're squishing something from star size (a million kilometers or miles, take your pick) to city-size (like, 25 kilometers or just 15 miles.) Plus, with all the interesting physics happening in the interiors, complex processes can operate to amplify the magnetic field. So you can imagine just how strong those fields get.

Actually, you don't have to imagine because I'm about to tell you. Let's start with something familiar: the Earth's magnetic field. That's around 1 gauss. It's not much different for the sun: a few to a few hundred gauss, depending on where on the surface you are. An MRI is 10,000 gauss. The strongest human-made magnetic fields are about a few hundred thousand gauss. In fact, we can't make magnetic fields stronger than a million gauss or so without our machines just breaking down from the stress.

Let's cut to the chase. A neutron star carries a whopping trillion gauss magnetic field. You read that right. I'm talking a trillion, with a t.

Enter the magnetar :
Now, we finally get to magnetars. You may guess from the name that they're especially magnetic: up to 1 quadrillion gauss. That's 1,000 trillion times stronger than the magnetic field you're sitting in right now. That puts magnetars in the number one spot, as the reigning champions in the universal Strongest Magnetic Field competition. The numbers are there, but it's hard to wrap our brains around them.

Those fields are strong enough to wreak havoc on their local environments. You know how atoms are made of a positively charged nucleus surrounded by negatively charged electrons? Those charges respond to magnetic fields. Not very much under normal conditions, but this ain't Kansas anymore, is it, Toto? Any unlucky atoms stretch into pencil-thin rods near these magnetars.

It doesn't stop there. With the atoms all screwed up, normal molecular chemistry is just a no-go. Covalent bonds cease to exist. Ha. And the magnetic fields can drive enormous bursts of high-intensity radiation. So, it's bad business generally.

Get too close to one (say, within 1,000 kilometers or about 600 miles,) and the magnetic fields are strong enough to upset not just your bioelectricity, rendering your nerve impulses hilariously useless, but your very molecular structure. In a magnetar's field, you just kind of dissolve.

We're not exactly sure what makes magnetars so frighteningly magnetic. Like I said, the physics of neutron stars is a little bit sketchy. It does seem, though, that magnetars don't last long, and after 10,000 years, give or take, they settle down into a long-term normal neutron star retirement: still insanely dense, still freaky magnetic, just not so bad.

So, as scary as they are, at least they won't stay that way for long.

About the author: Paul Sutter is a research fellow at the Astronomical Observatory of Trieste and a visiting scholar at The Ohio State University's Center for Cosmology and Astro-Particle Physics. Sutter is also host of the podcasts: Ask a Spaceman and RealSpace, and the YouTube series Space In Your Face. He contributed this article to's Expert Voices: Op-Ed & Insights.

Read: Black Hole birth of the universe
Center of a Black Hole
Falling down a Black Hole
Tachyons and Big Bangs

Now you know.

from the imagination of Mark A. Carter - writer

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