Radiocarbon (C14) Dating

The Basics
Of course you know how radiocarbon or C14 dating works on principle. I did credit you with a halfway decent education, remember? So in what follows I only want to refresh your memory.
The first thing to remember is that plants turn the carbon dioxide or CO2 contained in the air into solid organic stuff like barley (for making beer), leaves (for shading beer gardens), grass, cauliflower. Or worse, leeks, celery, Brussels sprouts and all kinds of salad. Then your wife (or kids if they study medicine like mine) force you to eat that.
Fortunately animals like chicken, cows and pigs also eat the plant stuff, turning it into something useful like steaks or ham which some of us also eat.
Whatever the food chain looks like in detail, one fact applies to everything that was once alive. As soon as something organic like you dies in some (hopefully far away) time in the future, or the tree you felled with your car, or the grass that withered in the sun, there is now some dead body around that contains a lot of carbon that came exclusively from the carbon dioxide in the air via the food chain.
Now something special happens. The carbon in the dead organic matter slowly changes over the years. And with carbon I mean the individual carbon atoms, no matter in what kind of molecules they find themselves as time goes by. When you're dead you rot and turn to compost but this involves only chemical reactions that change the molecules but not the atoms. The basic insight is that all the oxygen, hydrogen, phosphorous, nitrogen and so on atoms do not change at all - except for the carbon atoms.
We need to answer two basic questions now:
1. How can an atom change itself? There are two basic ways:
  1. The nucleus of an atom, the tiny assembly of protons and neutrons in the center of the atom, emits an elementary particle like an electron (b - decay), an helium nuclei (2 protons plus 2 neutrons; a - decay), a positron, or whatever. This is simply radioactive decay and what's left is a different atom.
  2. The nucleus of an atom gets hit by some energetic particle like a proton or a neutron in such a way that the composition of the nucleus changes. Sort of the revers of radioactive decay. A different atom is produced once more.
Advanced Link

Elementary particles
  You might wonder about the electrons surrounding any atom - what's their role in this? None. They just rearrange to whatever is needed. The energy involved for this is minuscule compared to what's going on in the nucleus and thus can be neglected.
2. How can some carbon atom be different from any other carbon atom?
  • It's called "isotopes", remember? The number of protons in a nuclei decide what element it is and thus is fixed, but the number of neutrons can be different for the same number of protons.
  • The nucleus of a carbon atom, for example, has always 6 protons (add 6 electrons and you have a carbon atom) but the number of neutrons can be 6, 7 or 8. That gives us three carbon isotopes: 12C, 13C, and 14C.
Basic Link

  The last thing to remember now is that some isotopes are stable forever, some decay radioactively. As it turns out, the carbon isotopes 12C and 13C are stable. 14C, however, decays with a halftime of 5 730 ± 40 years. In other words, if you start with 1 000 14C atoms, you will only have 500 left after 5 730 years. 250 after 2 ×5 730 years = 11 460 years, and so on.
  How It Works
All elements where made some time ago (like 10 billion years or so), either in the big bang or inside a sun. The ratio of the isotopes of a given element was fixed right then, and all the radioactive ones have long since disappeared (with a few exceptions that are of no interest here). The ratio of 12C to 13C thus is fixed at 99 : 1, and this ratio is immutable.
There is no 14C left over from the times when all the carbon atoms were made.
However, the atmosphere of our planet consists of 78.08% nitrogen molecules (N2), 20.95% oxygen molecules (O2), 0.93% argon (Ar), 0.038% carbon dioxide molecules (CO2) plus traces of other stuff of no importance here. What is of importance here is that all these molecules and atoms in the upper strata of the atmosphere get hit by highly energetic particles of the cosmic radiation that bombard the earth relentlessly all the time. The atmospheric layers up there stops most of this radiation. That is generally a good thing for normal people because we would not be here or last very long if we would be hit by that radiation.
It is also a good thing for archeologists because some of that radiation hits nitrogen atoms and turns them into the 14C isotope. The precise reaction is
n  +  14
N   Þ    15
N   Þ   14
C + p
In words: A nitrogen atom with (per definition) 7 protons and 7 neutrons (adding up to 14N) gets hit be a neutron (n) that was supplied by cosmic radiation, and turns into the unstable 15N isotope that decays immediately into 14C by emitting a proton (p).
In yet other words: In the upper atmosphere 14C is generated at a constant rate. It trickles down, forms carbon dioxide, and gets incorporated into plants and finally into everything alive. It decays inside you but as long as we live, we replenish it and essentially keep up a constant level of 14C in our organic bodies. As soon as we die, no more 14C is added to the remains and whatever was there now decreases in concentration by a factor of two every 5 730 years.
Radiocarbon dating now is easy. Measure the relative concentration of the14C isotope in living (or freshly dead) organic material, and you have the starting point. It is about 1 part per trillion, i.e. you have about 600 billion radioactive carbon atoms in one mol of carbon. A mol is a defined amount of stuff.
If the organic matter you unearthed somewhere (typically coal from some old fire, bones or wood remains; all containing carbon) happens to be 5 730 years old, you would find only half of that concentration or only 300 billion radioactive carbon atoms in one mol of carbon.
With a little simple math, the "Before Present" or BP age tBP of a sample comes out to
tBP   = – 5 730 years   ·  log2  N 
N is the measured 14C concentration; N / N0 thus the relative concentration of how much 14C is left. This follows straight from our old beer math.
Is that cool or what? So of course you know everything about the hero of science who came up with that monumental recipe for dating old organic things: Willard Frank Libby and his team at the University of Chicago first came up with the method in 1946; Libby got the Nobel price in 1960.
The basics are clear now. It only remains to look at the small print coming with the general recipe for 14C dating. We need to answer two big questions:
  1. How do you measure those extremely small amounts?
  2. How reliable are the results you get, or in other words: how large are the error margins and what determines their magnitude?
  How It Is Done
How is it done? Well - the stuff is radioactive after all! So get a Geiger counter or whatever else registers radioactive decay, hold it over your sample, and measure how many "clicks" you get per time unit (= N). Repeat with a sample of modern carbon that contains exactly as much carbon as the sample you want to date to give you the N0. Use the equation form above and you are done.
OK - that's how Libby did it, and there are problems, of course. From tiny samples you don't get that much signal, so your N value has an error of roughly N½. Your N0 value has an error - and how do you determine the exact weight you need (or just the exact carbon weight of your sample)? Than your halftime value may be a bit off. In fact, Libby used a value of 5568±30 years that was later corrected to 5730±40 years.
Maybe your sample as contaminated with a bit of "fresh" carbon? The tree those Greek guys used to barbecue their rabbit was a 500 year old oak that was felled by a flash of lightning - your are 500 years off the proper date of the fire! An so on.
The most tricky source of error, however, is that the 14C/12C ratio for "fresh" carbon is not really constant as was assumed as a matter of course. This may have several reasons:
  • Some of the cosmic radiation comes from our sun, and she is not totally reliable but wiggles the intensity a bit every now and then.
  • The magnetic field of the earth influences cosmic rays somewhat (it deflects them to some degree). The magnetic field of the earth changes on large time scales and so does the 14C/12C ratio.
  • The earth also exchanges carbon from the soil or from the oceans with the atmosphere at fluctuating rates, influencing the 14C/12C ratio.
  • And so on. Supernova explosions nearby may increase the cosmic radiation intensity for a while or maybe not. We just don't know.
Since we have some more methods to date things, and since more and more details become clear, we now have a calibration curve:
Radiocarbon calibration curve
As the examples show, a radiocarbon age of 20 000 (10 000) years translates into 23 900 (11 400) BP years or 21 900 (9 400) BC. So be careful about the BP and the BC! With this curve we get rid of the fluctuating 14C/12C ratio problem, at least to some extent. We are also rather certain that the halftime is now as correct as it can be. The only problem that remains is to measure the amount of 14C still there. That gets more difficult for old thing because most of it has already decayed and thus disappeared, and for very small specimen that do not contain much to start with. The decay rates then are so low that they do not register anymore in your Geiger counter or more sophisticated equipment.
That's when "accelerator mass spectrometry" (AMS) kicks in. This is rather tricky (and very expensive) but allows a far better analysis of the 14C/12C ratio for far smaller samples than the direct method.
  How does it work? You atomize your specimen, ionize the carbon (and whatever else will get ionized), accelerate those ions by high voltage, run them through a thin film to strip off electrons in order to destroy all charged molecules (like 13C1H) that might be in there and would be confused with 14C, accelerate the pure ions now once more with a really high voltage (several million Volts), and separate different atoms and their various isotopes by magnetic fields into individual ions beams. Measure how much 14C and 12C flies along and you have the ratio.
Here is an impression of what is involved (from the Leibniz Laboratory for Radiometric Dating and Stable Isotope Research of my University (Christian-Albrechts-University of Kiel, Germany).
Radiocarbon dating; Leibniz Labor Uni Kiel
Hardware for accelerator mass spectrometry
Doesn't look cheap, isn't cheap, and is not all that easy to operate. You need to know exactly what your are doing, in particular with respect to specimen preparation. The data you get are only as good as your specimen. Breath at it once in the wrong way, and its contaminated with fresh carbon, yielding faulty results.
Not sparing time and money, how good can it be? Well, after about ten half-lives, approximately 60,000 years, not much 14C is left (1/ 210) » 1/1 000). That gives sort of the lower limit for a 1 mg sample. Very young stuff is problematic too, but why should you want to date that?
  Pure iron, copper, gold and so on, not containing any carbon, cannot be dated this way at all, of course. But what about steel? It contains carbon and that we can dated. Yes - but where did that carbon come from? If it came exclusively from the charcoal used in the smelting process, you get the age of the tree the charcoal was made from, and that should be close enough. However, if some of the carbon came from the limestone or calcium carbonate (CaCO3) that was added for some reason, or if you used coal (from trees that died many million years ago) your results are useless.

With frame With frame as PDF

go to General Remarks to Literature and Sources

go to Elementary Particles

go to Beer

go to Diffusion in Iron

go to Israel Museum

go to Florence Museums

go to Landesmuseum für Vorgeschichte (Halle)

go to 10.2 Making Iron 10.2.1 Early Iron

go to The Ages

go to Phosphorous Steel; 9.4.1 General Remarks

go to 11.1.4 Swords of Major Near East Powers in the 1st Millennium BC

go to Isotopes

go to Early Copper Sites

go to Large Pictures 1

go to 11.4.2 Blades of Viking Era Swords

go to Large Pictures chapter 11.4

go to 10.3 Iron and Steel in Early Europe; 10.3.1 Technology Transfer and Trading

go to 11.1.3 The The Luristan Iron Sword

go to Dislocation Science

go to More Luristan Swords

go to Cayönü Tepesi

go to Entropy

go to Old Copper Complex of the Western Great Lake

go to Yumuktepe

go to Rosh Horesha, Shanidar Cave

go to Nevali Çori

© H. Föll (Iron, Steel and Swords script)