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Posted on August 10, 2004

Soapbox Seminar #5

A Black Hole Primer


Last time, we were saying that maybe the key to the whole Tunguska riddle lies in the nature of primordial black holes, like the one the Jackson-Ryan hypothesis claims hit the earth that morning in late June 1908. So, what is it about PBHs that, all evidence to the contrary, might help that claim prove out?

We’ll get there, trust me. For now, though, maybe it’s better if we back up a bit and talk about black holes in general. Begin at the beginning, so to say.

And, for a black hole, the beginning is gravity.

Now, the thing of it is, gravity’s just not much to write home about as forces of nature go. Compared to, say, the strong nuclear force, it’s a gossamer — the next best thing to nothing at all. Even plain old electromagnetism’s got it beat hands down. Ever pick up a three-penny nail with a toy magnet? Then you know how even a teensy bit of electromagnetic force can overcome the gravitational pull of the whole earth.

What you maybe never realized is, it’s that same disparity of forces that makes it possible for a planet like earth to exist in the first place.

Because, when you get right down to it, gravity does have one thing going for it — it just keeps on adding up.

And that’s pretty unique, for a long-range force. The strong and weak nuclear forces, for instance, they’re just too short-range to amount to much over the long haul. Electromagnetism’s got the reach, all right, but it comes in opposing flavors: positive and negative, north and south. That mostly puts a natural upper limit on how strong an electromagnetic field can get before it attracts enough opposite charges to neutralize itself. You can see that clearest on a subatomic scale: atoms normally have the same number of negatively-charged electrons and positively-charged protons, so they net out neutral. But it’s the same story for all the things built out of atoms, including the universe as a whole.

Gravity, on the other hand, only works one way. Never cancels out, never lets go. Each small chunk you add to an object’s mass can only increase, never diminish, the power of its gravitational field. Just by an infinitesimal amount, maybe, but still that field-strength is always growing, always pulling a little harder.

In the end, it’s only the fact that electromagnetism is so much stronger than gravity — about a million billion billion billion billion times stronger — that allows for kind of a Mexican standoff between the two forces. Take away the mutual repulsion of negatively-charged electron shells, and all the normal solid matter we know and love — rocks, trees, dachshunds, us, the earth itself — would implode in an instant into tiny little droplets of degenerate matter, dense as the core of the sun.

But there are times and places where even electromagnetism’s not up to the job: Pack a big enough mass into any one place — we’re talking really big here: say, a planet ten times the size of Jupiter — and the pressure at the core’ll exceed anything electromagnetism can stand up to. The electron shells that give things their structural strength just up and buckle. What started out as nice, solid matter dissolves into this sort of ‘soup’ of dissociated electrons and free nuclei.

That degenerate-matter soup is the first step on the road to making a black hole. But we’re not there yet, not by a long shot. Matter’s still got some fight left in it.

Take that super-Jupiter we were talking about. Once gravity overcomes its structural integrity, it starts to shrink. It’d keep right on shrinking, too, except compressing matter like that generates heat, and enough compression’ll heat the planet’s core to upwards of ten million degrees Kelvin. That’s the flashpoint: At that temperature, the free atomic nuclei are moving fast enough to overcome their mutual repulsion and start slamming into each other. The strong nuclear force takes over and thermonuclear fusion kicks in.

Fusing lighter elements into heavier ones releases energy. Massive amounts of energy. Enough energy to push back against the pull of gravity. Enough to light the heavens. Enough to warm the worlds and spark the chemical processes that lead to life, to us.

Enough to make stars.

Things can’t go on like that forever, of course. It takes fuel to keep those fires burning. Hydrogen to start with: A star’ll spend most of its lifetime transmuting hydrogen into helium. Works out well enough: hydrogen’s the most abundant element in the universe, after all. The average star holds enough to chug along for billions of years. But sooner or later it’s got to run out. And, when it does, the squeeze starts all over again.

Once gravitational contraction kicks in again, it raises the core temperature back up to where the fire rekindles. Only now the helium ‘ash’ itself becomes the fuel, fusing into heavier and heavier elements — carbon, lithium, oxygen, neon, silicon. All the while, though (if you can call millions of years a ‘while’), the star’s sliding down the slope of the binding-energy curve, earning less and less from each new element-building transaction, until it bottoms out at iron.

Far as nucleosynthesis is concerned, that’s all she wrote. End of the line: Finis. You can’t wring out any more watt-hours by turning iron into something else. Turning iron into any heavier element actually takes energy.

And that sets the stage for the final act.

At the very end there, gravity can grip hard enough that the core of the star just... collapses — collapses so fast, it rebounds. You get a gigantic explosion, a nova or supernova. The star puts out more energy in that blink of an eye than it did in a whole lifetime of steady shining. The shockwave is powerful enough to transmute elements wholesale and scatter them all across space. At its dying moment, the star seeds the universe with the building blocks of new worlds and new life.

In the aftermath, the only thing that matters is matter itself: namely, how much matter the explosion leaves behind. If what’s left over is only the mass of the sun or so, no problem: Atomic nuclei’ve got enough structural strength to bear that much weight. You wind up with a brown dwarf star the size of the earth, so dense that a teaspoon of its stuff weighs as much as a locomotive.

But upwards of one solar mass, things start to get interesting.

The leftovers don’t have to weigh too much more than the sun for the pressure in the interior to mash electrons and protons together. That gives you neutrons. And that triggers another collapse, into a neutron star only a few miles across. Bizarre enough in its own way, I suppose.

But the point where the relativity theorists really sit up and take notice is when the supernova ‘cinder’ is more than three times the mass of the sun. Not even neutrons can hold back that much gravity; they just up and cave. And neutrons are the last line of defense. Once they go, the whole mass collapses to what we call a singularity — a dimensionless point of infinite density, infinite space-time curvature, infinite you-name-it.

Gravity is just geometry. Imagine if three-dimensional space was a two-dimensional sheet of rubber. That’d make gravity the measure of how much that rubber sheet stretches when you put a mass on it — less for a marble than for a bowling ball. Drop a planet-sized mass onto that rubber sheet and the nearby space curves in to form a gravity well steep enough for moons to roll in orbit around it. Drop in a sun, and the deformation dips deep enough to trap a family of planets in its folds.

But that same geometry is destiny. When a really massive star dies, the sink-hole round its corpse plunges infinitely deep. The well-walls wrap around and pinch shut, sealing off the remains from the rest of space-time. Remember Alice in Wonderland, where the Cheshire Cat vanishes, leaving only its smile behind? Well, here, the matter disappears, and only the mass is left. In the process, the gravity gradient grows so steep that nothing, not even light, can escape ...

... which is why we call them black holes.

copyright (c) 2004 by amber productions, inc.


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Mitchell Begelman and Martin Rees, Gravity’s Fatal Attraction: Black Holes in the Universe, Scientific American Library, 1996.

Kitty Ferguson, Prisons of Light — Black Holes, Cambridge University Press, 1996.

Stephen Hawking, Hawking on the Big Bang and Black Holes, World Scientific (Advanced Series in Astrophysics and Cosmology, Vol 8), 1993.

Igor Novikov, Black Holes and the Universe?, Cambridge University Press, 1990.

Kip S. Thorne, Black Holes and Time Warps: Einstein’s Outrageous Legacy, Norton, 1994.


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copyright (c) 2004 by amber productions, inc.