carbon 13

The atomic nucleus is not a bag of marbles but an ordered structure where protons and neutrons fill shells, much like electrons in an atom. When a shell is filled, the nucleus becomes especially stable, and the number of particles is called magic. For calcium with 20 protons, the classic magic neutron numbers are 20 and 28.

The atomic nucleus is usually pictured as a dense ball where protons and neutrons are mixed together. But in some isotopes, neutrons can stick out far beyond this ball, forming a diffuse shell — a neutron halo. This is especially common in nuclei with many more neutrons than protons.

An extra electron in a molecule is like a passenger barely hanging onto the step of a departing train. Such a 'passenger' turns the particle into an anion — a negative ion. Studying it is tough: the bond is weak, the electron cloud is diffuse, and any jolt can knock the electron off.

A star's radius drops by a thousand kilometers. Not because its mass increased, but because its own magnetic field squeezed the crust like an invisible corset.

An atomic nucleus is not just a ball of protons and neutrons. It has a shape, and that shape can change. The tin-116 nucleus was long considered almost perfectly spherical: it has 50 protons — a 'magic' number that usually gives a nucleus spherical symmetry. But a new ultra-precise measurement showed otherwise.

In 1905, Einstein showed that the chaotic motion of pollen in water results from the jostling of invisible molecules. A century later, physicists have learned not only to observe but also to control motion at the quantum level.

Trying to count people in a dark room by the sound of their breathing hits a wall of background noise — individual breaths are inaudible. Scientists working with quantum spins in solids face a similar challenge. Each spin (the electron's magnetic moment) has its own "voice," but it is drowned out by the technical noise of the instruments.

Neutrinos are often compared to a radio broadcast picked up by different receivers. One station sends a signal, but antennas in Japan, Antarctica, and at the bottom of the Mediterranean Sea hear it differently — due to distance, interference, and antenna orientation.

Two neutron stars whirl in their final dance. If their spin aligns with their orbital motion, the partners merge neatly, launching a narrow jet of superheated matter. If they spin in opposite directions, the dance breaks apart, scattering a thick shroud of debris.

Atomic nuclei are wrapped in fluffy electron coats — in such attire, they can't get close enough to embrace. But swap the light coat for a heavy one: a muon, a particle from the standard model, shrinks the cloud by nearly 200 times.

Quantum networks need a mediator between storage — spin — and carrier — light. No single molecule had ever pulled off such a feat. But now physicists have found a solution. They placed a carbene molecule into a crystal and cooled it to -269°C.

A substance's spectrum is its fingerprint. Usually, to record one, you place the sample in a strong magnetic field, like in an MRI scanner. But there is a way to do without a magnet altogether: detect the signal from atomic nuclei at zero field. Until now, this method suffered from poor sensitivity, and its complex spectra were hard to predict.

Imagine a multi-story building where protons and neutrons live on each floor. The floors are energy levels, and usually there's a stairwell of a certain height between the sixth floor and the one above — the so-called gap. In the oxygen-20 nucleus, this gap acts as a barrier that particles find hard to cross.

The atomic nucleus is not just a ball of protons and neutrons. Inside it, like a tiny magnet, there is its own distribution of magnetization. Until now, it has been difficult to see: nuclei live for tiny fractions of a second, and their magnetic field is weak. Now physicists at CERN have found a way to look inside.

Deep inside a dying star, just before it goes supernova, nuclear reactions determine which chemical elements will be scattered across the cosmos. One such reaction is the collision of an oxygen nucleus with a proton, producing a nitrogen nucleus and an alpha particle (a helium nucleus).

An atomic nucleus usually follows its own rules: its decay doesn't care about temperature, pressure, or molecular neighbors. But the uranium-235m isotope is a striking exception. This nucleus sits in an excited state, like a tightly coiled spring, and sooner or later it releases the extra energy.

Silicon is like a universal building block: it goes into the chips in your phone, solar panels, and lasers. But if you squeeze it with immense force, the atoms rearrange into new patterns: these forms are called allotropes. One of them, Si-XIII, was first spotted more than twenty years ago, but its exact pattern remained a mystery.

A quantum computer is like an orchestra where electrons and nuclei play different instruments. Usually, the conductor needs two batons: microwaves for electrons and radio waves for nuclei.

A bell doesn't ring with a single note — after being struck, it sounds with several harmonics at once. An atomic nucleus vibrates in much the same way: after a collision, it can oscillate, and these oscillations show up in the emitted gamma rays.

A magnetic compass in a test tube sounds like a magic trick, but it's pure physics. In a solution of fumarate (a salt of malic acid), carbon-13 nuclei behave like tiny spinning tops.

At the center of many galaxies lurks a black hole — an object predicted by solutions to the equations of Karl Schwarzschild. Around it stretches a scorching corona — a region of tenuous plasma heated to billions of degrees.

Deep inside stars, light nuclei fuse, giving birth to helium and streams of neutrons. On Earth, we recreate this process by combining deuterium and tritium — special isotopes of hydrogen.

In a laboratory at Purdue University, a laser beam strikes a crystal of hexagonal boron nitride, and in response, a single point of light flashes. This is not just luminescence; it is a signal from a spin defect, a pair of electron spins, one of which is coupled to a carbon-13 nuclear spin.

Inside a diamond, you sometimes find tiny flaws — a spot where a carbon atom is replaced by nitrogen, with a vacancy right next to it. Physicists call this an NV center (a nitrogen-vacancy defect). Such a defect acts like a magnetic needle that can store information in its spin.

A tuning fork sounds when you strike it. Its prongs vibrate, and you hear the sound until the vibration dies out. The quantum world has its own "tuning forks"—for example, a defect in diamond that responds to magnetic fields, and a carbon tube that can tremble at frequencies billions of times higher than the note A.

Hidden within the bulk of a diamond are tiny flaws — places where a carbon atom is replaced by nitrogen, with a vacancy gaping nearby. These defects, like beacons, can store and transmit quantum information. But around them rages a magnetic storm: the nuclei of atoms in the crystal jostle, creating interference.