ultra high energy gamma ray

On the lab bench lies a piece of graphite grown from gas, like a deposit on the wall of a reactor. Usually, such material is not suitable for converting heat into electricity: inside it, electrons and holes run in opposite directions and cancel each other out.

An assembly line spits out parts one by one per cycle. If the cycle is short and defects are few, the line runs fast. In quantum optics, a single-photon source plays the role of such a line: it must emit exactly one quantum of light per cycle, and the more cycles per second, the more photons go into the fiber.

A cartographer receives a sheet with distances between hundreds of unnamed islands. No island is labeled, but the distances repeat, forming triangles and quadrilaterals. From these repetitions, the cartographer reconstructs the map of the archipelago, not knowing which island is which. This is roughly how the new work in molecular spectroscopy works.

A gas target is like a funnel: the steeper its walls, the stronger the flow. But in this funnel, it is not water that flows, but ultraviolet light, born when a powerful laser pulse passes through a cloud of argon. The efficiency of this conversion is usually minuscule, about 0.001%: out of a thousand laser photons, only one turns into useful ultraviolet.

The blue glow in water around a nuclear reactor is light born when a charged particle outruns light in that medium. The effect was discovered by Pavel Cherenkov in 1934, with the theory provided by Igor Tamm and Ilya Frank.

In 1054, a star flared up in the constellation Taurus. The light of its death was so bright that it was visible in daylight for nearly a month, and Chinese astronomers recorded it in their chronicles. Today, the Crab Nebula is spreading over that spot, and its claws are clouds of gas still being whipped up by the dead star at its center.

Imagine a huge stadium packed with people dressed in black. You're standing outside, trying to figure out what's happening inside, even though you can't see a single person. But if two people bump into each other and exchange bright T-shirts, you'd spot a flash of color.

In the first moments after the Big Bang, the universe expanded at an incredible rate — a phase known as inflation. Even the vacuum was restless back then: quantum jitters shook the fields like wind rustling through a wheat field.

For a long time, astronomers searched for the 'factories' of the most energetic cosmic rays — particles that carry the macrocosm compressed to the size of an atomic nucleus. Colossal star-forming regions like Cygnus OB2, where winds from young giants collide, were prime suspects.

In the constellation Aquila, about 40,000 light-years away, one of the most powerful natural accelerators in the Galaxy is at work. It's the microquasar GRS 1915+105—a pair consisting of an ordinary star and a black hole.

The giant galaxy cluster Abell S1063, lying 4 billion light-years away, works not just as a lens but as a gravitational well of time. Its mass bends space so sharply that photons from an era when the Universe was just 500 million years old slide along curved paths, like rays in slow motion, and converge on us magnified forty-three times.

Gravitational waves are ripples in the very fabric of spacetime, akin to vibrations of a giant cosmic string. Conventional detectors like LIGO and Virgo pick up low-frequency "notes"—disturbances from mergers of massive black holes of stellar masses.

Blacksmith's bellows fan the fire by forcefully pushing out air. In space, the shock wave from a supernova, a concept introduced by Fritz Zwicky, acts like such bellows: it catches up with a giant bubble of charged particles and magnetic fields formed around a spinning neutron star…

At the heart of the Galaxy, about 7 kiloparsecs away, lies a true natural particle accelerator. This is a rapidly spinning neutron star — the pulsar PSR J1849-0001, left behind by a supernova explosion.

A factory laser that cuts and welds metal on production lines has been made to work as a particle accelerator for the first time. Physicists took a standard ytterbium laser, its heart is a crystal the size of a palm, and turned its flashes into a tool for accelerating electrons to nearly the speed of light.

Elliptical galaxies are quiet stellar metropolises in retirement. By all rights, their light should be calm, reddish, like a sunset. But their spectra scream otherwise: in the far ultraviolet, these old-timers blaze like holiday lights. For three decades, astronomers have puzzled over this 'ultraviolet upturn' (UV upturn).

Dark matter is an invisible substance that reveals itself only through gravitational effects: it bends the light of distant galaxies, much like an unseen window that alters the path of light rays.

A spotlight shines ever brighter, but at some limit the bulb suddenly burns out, and no more light comes through. Astrophysicists have seen something similar in the distant blazar Markarian 421. This is an active galaxy whose jet of superheated plasma points almost straight at Earth, like the beam of a cosmic lighthouse.

Cosmic rays are particles from deep space, accelerated to colossal energies. Smashing into the atmosphere, they trigger particle showers with radio waves. These waves are fingerprints, revealing the energy and direction of the intruder.

A detector filled with superfluid helium-4 is like a perfectly still lake. The liquid doesn't slosh or bubble: it's frozen in a single quantum state. An invisible guest, a dark matter particle, flies through it. It doesn't shine or leave a track. But sometimes it nudges a helium nucleus.

An alpha particle is a helium nucleus that flies out when heavy atoms decay. When it hits a gallium nitride crystal, it deposits its energy and creates an electrical pulse. The pulse height tells you how much energy the particle had.

An ordinary laser emits narrow lines, like a string that sounds only one note. For spectroscopy, this is inconvenient: if a substance absorbs light between the lines, you might miss it.

Every second, invisible projectiles from the depths of space pierce through us. These are cosmic rays — atomic nuclei accelerated to speeds nearly indistinguishable from the speed of light. Their energy is hundreds of millions of times greater than what our most powerful accelerators can achieve. Where does this monstrous force come from?

The speed of light in a vacuum is physics' metronome: it sets the rhythm for all processes. If it falters, the familiar harmony collapses. Neutrinos, ubiquitous but almost intangible particles from space, can check if this rhythm ever stumbles under extreme conditions.

In a distant galaxy, at a distance that light takes 11 billion years to cross, something flashed. The Einstein Probe X-ray telescope caught a brief, needle-prick-like burst: it lasted only a few dozen seconds.

Gamma-ray burst GRB 221009A flared so brightly that it was dubbed the 'brightest of all time.' The LHAASO observatory detected gamma rays from it with energies up to 13 TeV — thousands of times more energetic than particles in an X-ray machine.

Electrons in a crystal sometimes behave like a stadium crowd doing the wave: areas of higher density alternate with nearly empty ones. This wave blocks the free flow of charges — under normal conditions, the material is not superconducting. But apply pressure, and the wave vanishes, letting electrons move without resistance.

The night sky looks still, but many stars tremble like a drum after a strike. For seven straight years, the TESS satellite stared at the same patches of sky and caught this trembling in 19,151 red giants — old, bloated stars. Previously, far fewer of these 'singing' giants were known, and now the list has grown by 80%.

An electron beam in an accelerator is like a flock of birds: it flies in a tight group, but over time it spreads out. To keep particles together, heavy magnets are usually used. Here they did without them — the beam squeezed itself.

Light in an optical fiber is a stream of photons, and quantum communication requires single photons that can be sent one at a time. But making them emerge quickly while remaining indistinguishable from one another is a tough challenge.

A shock wave in the Sun's corona is like the sonic boom from an airplane, except instead of air there is scorching plasma, and instead of sound there is a jump in density and magnetic field. On March 10, 2024, such a wave swept across the western part of the solar disk.

For 17 straight years, the Fermi space telescope recorded light from the distant galaxy 4C 76.03. Most of the time, it behaved quietly, like a night city with only a few lit windows. But in the observation archive, two brief moments stood out when the galaxy flared in gamma rays — the most energetic light in the universe.

The black hole in V4641 Sagittarii behaves like a vacuum cleaner running at full power, but neighbors only see a faint indicator light. The LHAASO and HAWC telescopes caught gamma rays from it with energies up to 0.8 PeV — millions of times more energetic than hospital X-rays.

Gamma rays with energies above one hundred trillion electronvolts are like stones thrown with incredible force. For a long time, it was believed that only protons, heavy particles accelerated in cosmic accelerators, could launch such 'stones.' But new work shows that sometimes light electrons are enough.

Deep in the constellation Aquila lies a nebula that looks like an expanding bubble. It is inflated by a tiny star the size of a city — a pulsar that makes several rotations per second and loses rotational energy. Usually, such bubbles shine exactly as brightly as their pulsar is powerful.

A gamma-ray burst is like a shot from a cosmic cannon: a brief but dazzling flash that outshines an entire galaxy for a few seconds. But when observed in the hardest gamma-ray band (photons with energies above a gigaelectronvolt), the signal often gets lost in the noise, like a whisper in a noisy hall.

Radiation therapy is like shooting at a small target with a very large-caliber rifle: even a precise shot hits a large area around it. The thickness of the 'trace'—called the penumbra — is 2–3 millimeters in standard machines. For a tumor in the lung, that's not a big deal, but next to a nerve or a blood vessel, those millimeters decide whether a person stays healthy.

Twenty-eight seconds: that's how long it took for an automated camera to lock onto a flash in a constellation whose light had traveled for more than nine billion years.

The binary system SS433 is known for its black hole stripping matter from a neighboring star. Some of the gas falls into the hole, while the rest is ejected in two narrow jets that wobble like a spinning top. These jets are visible in radio and X-rays.

An ordinary free-electron laser is like a musical instrument with a single string: it can play only one note until you change its design. To get a different wavelength, you have to retune magnets or accelerate electrons harder. That's expensive and bulky.