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Starts With A Bang

Why The Unexpected Muon Was The Biggest Surprise In Particle Physics History

Cosmic rays, which are ultra-high energy particles originating from all over the Universe, strike protons in the upper atmosphere and produce showers of new particles. The fast-moving charged particles also emit light due to Cherenkov radiation as they move faster than the speed of light in Earth’s atmosphere, and produce secondary particles that can be detected here on Earth. (SIMON SWORDY (U. CHICAGO), NASA)

Science was never the same after meeting ‘the particle who lived.’


Back in the early 1930s, there were only a few known fundamental particles that made up the Universe. If you divided up the matter and radiation we observed and interacted with into the smallest possible components we could break them up into at the time, there were only the positively charged atomic nuclei (including the proton), the electrons that orbited them, and the photon. This accounted for the known elements, but there were a few anomalies that didn’t quite line up.

Heavier elements also had more charge, but argon and potassium were an exception: argon only had a charge of +18 units, but a mass of ~40 atomic mass units, while potassium had a charge of +19 units, but a mass of ~39 units. The 1932 discovery of the neutron took care of that one. Certain types of radioactive decay — beta decays — appeared to not conserve energy and momentum, leading to Pauli’s 1930 hypothesizing of the neutrino, which wouldn’t be discovered for another 26 years. And the Dirac equation predicted negative energy states, which corresponded to antimatter counterparts for particles like the electron: the positron.

Still, nothing could have prepared physicists for the discovery of the muon: an unstable particle with the same charge, but hundreds of times the mass, of the electron. Here’s how this surprise really did turn physics on its head.

The electric charge on an electroscope, depending on what you charge it with, and how the metal foil leaves inside respond. If the leaves remain charged, the two foil leaves will repel. If the leaves are uncharged, they will simply fall down. What was remarkable is that electroscopes, even if placed in a vacuum, will discharge over time. The reason why was not obvious, but is due to cosmic rays. (BOOMERIA’S HONORS PHYSICS PAGE)

The story starts way back in 1912, when adventuresome physicist Victor Hess had the brilliant idea to take a particle detector with him on a hot air balloon flight. You might wonder what the motivation would be for this, and it came from an unlikely source: the electroscope (above). An electroscope is just two thin pieces of conducting, metal foil, connected to a conductor and sealed inside an airless vacuum. If you charge up the electroscope, either positively or negatively, the like-charged pieces of foil will repel each other, while if you ground it, it becomes neutral, and goes back to the uncharged position.

But here was the strange thing: if you left the electroscope alone, even in a fairly perfect vacuum, it still discharged over time. No matter how good you made your vacuum — even if you placed lead shielding around it — the electroscope still discharged. Moreover, if you performed this experiment at higher and higher altitudes, it discharged more quickly. This was where Hess got his big idea, imagining that high-energy radiation, with both high penetrating power and of extraterrestrial origin, was the culprit.

By taking a hot air balloon up to high altitudes, far higher than could be achieved by simply walking, hiking, or driving to any location, scientist Victor Hess was able to use a detector to demonstrate the existence and reveal the components of cosmic rays. In many ways, these early expeditions, dating back to 1912, marked the birth of cosmic ray astrophysics. (AMERICAN PHYSICAL SOCIETY)

If there are charged cosmic particles zipping through Earth’s atmosphere, they could help neutralize this charge over time, as the oppositely-charged particles would be attracted to the electrode and the like-charges would be repelled by it. Hess imagined that there was a very real “zoo” of particles zipping around through space, and that the closer he got to the edge of Earth’s atmosphere (i.e., the higher altitudes he went to), the more likely he’d be to observe these particles directly.

Hess constructed a detection chamber that contained a magnetic field, so that any charged particles would curve in its presence. Based on the direction and curvature of any particle tracks that appeared in the detector, he could reconstruct what the velocity of the particle was as well as its charge-to-mass ratio. Hess’s earliest efforts immediately paid off, as he began discovering particles in great abundance, founding the science of cosmic ray astrophysics in the process.

The first muon ever detected, along with other cosmic ray particles, was determined to be the same charge as the electron, but hundreds of times heavier, due to its speed and radius of curvature. The muon was the first of the heavier generations of particles to be discovered, dating all the way back to the 1930s. (PAUL KUNZE, IN Z. PHYS. 83 (1933))

Many protons and electrons were seen in these early cosmic rays, and later on, the first antimatter particles were discovered this way as well. But the big surprise came in 1933, when Paul Kunze was working with cosmic rays and found a particle that didn’t quite fit. It had the same charge as an electron, but was simultaneously far too heavy to be an electron while also being far too light to be an antiproton. It was as though there was some new type of charged particle, of an intermediate mass between the other known particles, that suddenly announced, “hey, surprise, I exist!”

The higher in altitude we went, the more cosmic rays we observed. At the highest altitudes, the overwhelming majority of cosmic rays were neutrons and electrons and protons, while only a small fraction of them were muons. However, as detectors got more and more sensitive, they started to be able to detect these cosmic rays at lower altitudes, even closer to sea level. Today, for about $100 and with off-the-shelf materials, you can build your own cloud chamber and detect cosmic ray muons — the most abundant cosmic ray particle at sea level — at home.

The V-shaped track in the center of the image arises from a muon decaying to an electron and two neutrinos. The high-energy track with a kink in it is evidence of a mid-air particle decay. By colliding positrons and electrons at a specific, tunable energy, muon-antimuon pairs could be produced at will. The necessary energy for making a muon/antimuon pair from high-energy positrons colliding with electrons at rest is almost identical to the energy from electron/positron collisions necessary to create a Z-boson. (THE SCOTTISH SCIENCE & TECHNOLOGY ROADSHOW)

Over the next few years, scientists worked hard to detect these muons not from high-altitude experiments, but to observe them in a terrestrial laboratory. In theory, they were being produced by what we call cosmic ray showers: where particles from space hit the upper atmosphere. When this occurs, interactions from the fast-moving cosmic particles that strike the stationary atmospheric particles produce lots of new particles-and-antiparticles, with the most common product being a short-lived, unstable particle known as a pion.

The charged pions live only for nanoseconds, decaying into muons, among other particles. These muons are also short-lived, but much longer-lived than the pion. With a mean lifetime of 2.2 microseconds, they’re the longest-lived unstable particle except for the neutron, which has a mean lifetime of around 15 minutes! In theory, not only should these cosmic ray showers produce them, but any collision of particles that had enough energy to produce pions should also yield muons that we could study in a lab. The muon, in our detectors, look just like electrons do, except they have 206 times the electron’s mass.

Cosmic ray shower and some of the possible interactions. Note that if a charged pion (left) strikes a nucleus before it decays, it produces a shower, but if it decays first (right), it produces a muon that will have a chance to reach the surface. Many of the ‘daughter’ particles produced by cosmic rays include neutrons, which can convert nitrogen-14 into carbon-14. (KONRAD BERNLÖHR OF THE MAX-PLANCK-INSTITUTE AT HEIDELBERG)

In 1936, Carl Anderson and Seth Neddermeyer were able to distinctly identify populations of both negatively and positively charged muons from cosmic rays, an indication that there were muons and anti-muons, just as there were electrons and anti-electrons (positrons) found in nature. The next year, 1937, saw the scientist team of J.C. Street and E.C. Stevenson independently confirm that discovery in a cloud chamber. Muons were not only real, but relatively common.

In fact, if you hold out your hand and point your palm so that it faces up, towards the sky, approximately one muon (or anti-muon) will pass through your hand with each second that goes by. At sea level, 90% of all the cosmic ray particles reaching Earth’s surface are muons, with neutrons and electrons making up most of the rest. Before we had even discovered mesons, which are composite quark-antiquark combinations, exotic, heavy, unstable baryons (which are combinations of three quarks, like protons and neutrons), or the quarks that underlie matter, we had discovered the muon: the heavy, unstable cousin of the electron.

The particles and antiparticles of the Standard Model are predicted to exist as a consequence of the laws of physics. Although we depict quarks, antiquarks and gluons as having colors or anticolors, this is only an analogy. The actual science is even more fascinating. Note how the particles come in three generations, or copies, with only the first generation giving rise to stable particles. (E. SIEGEL / BEYOND THE GALAXY)

As soon as the physicist I. I. Rabi, who himself would win the Nobel Prize for the discovery of nuclear magnetic resonance (today used ubiquitously in MRI technology), learned about the muon, he famously quipped, “who ordered that?” With so few particles known at the time, adding this strange cousin of the electron — heavy, unstable, and short-lived — seemed like a phenomenon of nature that defied explanation.

We were decades away from uncovering the nature of matter and the structure of the Standard Model, but the muon was our very first clue that there were not only more particles out there waiting to be discovered, but that particles came in multiple generations. The first-generation of particles are the stable ones, consisting of the up and down quarks, the electron and the electron neutrino, and their antimatter counterparts. Today, we know of two more generations: the second-generation, which has charm and strange quarks with muons and muon neutrinos, and the third-generation, which has top and bottom quarks with tau and tau neutrino particles, plus their analogous antimatter counterparts.

At high enough energies and velocities, relativity becomes important, allowing many more muons to survive than would without the effects of time dilation. As it stands, approximately 25% of the muons created in the upper atmosphere reach the Earth. Without relativity, that number would be something like 1-in-1⁰²⁰. (FRISCH/SMITH, AM. J. OF PHYS. 31 (5): 342–355 (1963) / WIKIMEDIA COMMONS USER D.H)

The muon, however, didn’t merely foreshadow all of these new discoveries, but it also yielded an exciting and counterintuitive demonstration of Einstein’s relativity. The muons that get created from cosmic ray collisions, on average, originate at an altitude of 100 kilometers. However, the mean lifetime of a muon is only 2.2 microseconds. If a muon moved extremely close to the speed of light at 300,000 km/s, you can do a little math, multiplying that speed by the muon’s lifetime, to find that they should travel about 660 meters before decaying.

But muons arrive at Earth’s surface, journeying 100 kilometers and still not decaying! How is this possible? Without relativity, it wouldn’t be. But relativity brings along the phenomenon of time dilation, enabling particles that move close to the speed of light to experience time passing more slowly than they do for observers at rest. Without time dilation, we would never have discovered these cosmic muons, and we wouldn’t be able to see them in our terrestrial cloud chambers, not unless we created them from particle accelerators. Einstein, despite not knowing it, helped us discover this fundamentally new form of matter.

An earlier design plan (now defunct) for a full-scale muon-antimuon collider at Fermilab, the source of the world’s second-most powerful particle accelerator behind the LHC at CERN. Muons could achieve energies comparable to protons, but with clean collision signals and all the energy concentrated into one point, like electrons. It truly could be the best of both worlds. (FERMILAB)

Looking ahead, being able to control and manipulate these muons just might lead to advances in experimental particle physics that no other type of collider can match. When you build a particle accelerator, there are only three factors that determine how energetic your collisions are:

  1. how big your ring is, with larger circumference rings achieving higher energies,
  2. how strong your magnetic fields that bend your charged particles are, with stronger magnets leading to higher energies,
  3. and the charge-to-mass ratio of your particle, with low masses leading to synchrotron radiation and a limiting energy, and high masses not having that problem.

That third factor is why we use protons instead of electrons in accelerators like the Large Hadron Collider at CERN, but there’s a drawback: protons are composite particles, and only a tiny fraction of its total energy winds up in a quark or gluon that collides with another. But the muon doesn’t suffer from that drawback, and it also isn’t limited by synchrotron radiation like electrons are, due to its much heavier mass. If we can master muon accelerators, we just might unlock the next frontier in experimental particle physics.

The Muon g-2 electromagnet at Fermilab, ready to receive a beam of muon particles. This experiment began in 2017 and was slated to take data for a total of 3 years, reducing the uncertainties significantly. While a total of 5-sigma significance may be reached, the theoretical calculations must account for every effect and interaction of matter that’s possible in order to ensure we’re measuring a robust difference between theory and experiment in the muon’s magnetic dipole moment. (REIDAR HAHN / FERMILAB)

Today, we can look back on the discovery of the muon as quaint, with our hot air balloons and primitive detectors revealing these uniquely bent particle tracks. But the muon itself continues to provide a legacy of scientific discoveries. From its power in illustrating the effects of time dilation on a particle’s observed lifetime to its potential to lead to a fundamentally new, superior type of particle accelerator, the muon is a whole lot more than just background noise in some of our most sensitive, underground experiments searching for the rarest particle interactions of all. Even today, the experiment to measure the muon’s magnetic dipole moment could be the key that takes us, at last, into understanding physics beyond the Standard Model.

Still, when it unexpectedly announced its existence in the 1930s, it was truly a surprise. For all of history before then, no one had imagined that nature would make multiple copies of the fundamental particles that underpinned our reality, and that those particles would all be unstable against decays. The muon just happens to be the first, lightest, and longest-lived of all of those particles. When you think of the muon, remember it as the first “generation 2” particle ever discovered, and the first clue we ever got as to the true nature of the Standard Model.


Starts With A Bang is written by Ethan Siegel, Ph.D., author of Beyond The Galaxy, and Treknology: The Science of Star Trek from Tricorders to Warp Drive.


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