eccentric black hole binary

In 2015, the LIGO detectors caught the first ripple of spacetime from a black hole merger. Since then, hundreds of such events have piled up, each carrying the imprint of its ancestry: whether the holes were born together from a single pair of stars or met by chance in a dense cluster. The difference shows in the direction of their spin axes.

A network of radio telescopes scattered across the planet catches the whisper of a distant black hole. Each antenna records a signal, but how do you combine these recordings if the clocks at the stations tick at different rates and the atmosphere distorts incoming waves?

Somewhere in the depths of space, two supermassive black holes are circling each other. Their dance is not smooth — the orbit is stretched, like a rubber band that alternately tightens and relaxes. Each revolution sends ripples through the fabric of spacetime — gravitational waves.

The quantum world does not forgive forgetfulness. Throw a stone into a pond — the ripples spread and vanish, the information about the impact dissipates without a trace. In quantum mechanics, everything is different: the evolution of a system is reversible, and the past is never completely erased.

Take two thin sheets of a semiconductor. One is saturated with free electrons, like a packed café where every table is taken. The other, by contrast, is full of empty spots—'holes' eager to be filled. When these sheets are brought close together, a spark of attraction jumps between them: electrons and holes begin to feel each other across the thin gap.

Two black holes circle in a cosmic dance, spiraling closer together. In the end, they merge into one, and that moment unleashes a powerful burst of gravitational waves, ripples in spacetime itself. But what remains after the merger?

Hidden within thin layers of tantalum selenide (TaSe₂) is a property that defies conventional physics. When guest atoms were added between the layers of this material, the structure lost its center of symmetry, and inside, superconductivity with armor emerged.

A gas disk with a mass of four hundred thousand suns encircles the black hole at the center of the Milky Way. Its gravity works like a gravitational rudder: slowly but inexorably turning the orbits of binary stars, driving them into the region where tidal forces tear the pair apart.

In May 2020, the LIGO and Virgo detectors picked up a gravitational-wave burst known as GW200105. Among the many similar gravitational waves recorded, this one stood out for an oddity: the orbit of the colliding neutron star and black hole was not a perfect circle, but a stretched ellipse.

At the center of a galaxy, a huge black hole is shrouded in an invisible cloud — a swarm of ultralight particles that it itself spawned. Into this cloud dives another black hole, about the size of a star, and begins a long spiral dance. The approach takes millions of years, but the most dramatic events unfold right at the horizon.

Two black holes spiraling toward each other resemble figure skaters in a pair spin: each rotates about its own axis, and together they weave a shared dance. This collective twist, the so-called effective spin, can be measured by astronomers from the gravitational waves rippling outward from the pair, like ripples on a pond.

In the dense core of a star cluster, three black holes converge in a dangerous dance. The motion is chaotic — trajectories tangle like balls of yarn. Then one hole is ejected, while the other two remain on an elongated orbit. Such a pair continues to spiral inward and eventually merges, producing a burst of gravitational waves.

Picture a tightrope walker balancing over an abyss. Every step changes the rope's tension, and the slightest shift in center of gravity can prove fatal. That's roughly what the dance of an ordinary sun-like star around a black hole of ten solar masses looks like when the orbit is highly elongated.

Many black holes are surrounded by magnetic fields. As it spins, the black hole drags curved spacetime along with it, like a machine's flywheel, and sets the cosmic factory in motion.

Two heavy spheres circle not in a neat circle but in a highly flattened oval — now approaching, now flying apart. That's roughly how pairs of black holes on elongated orbits behave. Unlike calm pairs that gradually spiral together and merge, these dancers retain a memory of their turbulent youth: of being kicked out of star clusters or made to whirl by close neighbors.

When a neutron star and a black hole merge, they send out gravitational waves — ripples in spacetime that reach Earth. These ripples carry the imprint of their final dance: the orbit before the collision is often elongated, like an ellipse.

An orchestra of millions of instruments plays a single note, but each enters at its own moment and with its own volume. That's how the stochastic gravitational wave background sounds — a hum from black hole mergers that are individually indistinguishable.

A pair of figure skaters spins while holding hands. If their path is a perfect circle, each push from a partner is predictable. But stretch that path into an oval, and the effort becomes uneven: a jerk as they come together, a lull as they pull apart. Something similar happens with two black holes in the final minutes before they merge.

Astronomers pointed JWST at a planet near the star Epsilon Indi — a giant gas ball resembling Jupiter, just 12 light-years away. In thermal images, the planet shone like a lantern. But nearby they noticed a faint dot — like a firefly. Calculations showed that two objects describe the picture better than one. However, it's most likely a lens flare — like a ghost of a lamp.

Two black holes spiral around each other not in a smooth dance, but like two stones thrown from opposite banks into a deep whirlpool. Their orbit resembles a highly flattened oval — the eccentricity is nearly one. When they finally collide, a powerful burst of gravitational waves is born — a shudder of space itself.

Every 15 hours, in a constellation 57 light-years away, a miniature solar eclipse takes place. A tiny white dwarf — a star the size of Earth but heavier than the Sun — ducks behind the disk of a red dwarf. For astronomers, this is not just a pretty coincidence but a way to peek into the pair's past.

Water in a kettle, as it boils, clearly separates into liquid and steam. But under enormous pressure, the boundary vanishes: the substance enters a supercritical state — neither one nor the other, but something in between. Black holes can do this too.

In the galaxy NGC 1566, located in the constellation Dorado, there is an active nucleus — a supermassive black hole surrounded by a cloud of fast-moving gas. As the gas falls toward the hole, it heats up and emits bright spectral lines. Sometimes these lines become very broad — a sign of the gas's rapid rotation.

The Kepler telescope spent years watching thousands of stars, spotting planets by the tiny dips in starlight when a planet passes in front of its star. Such a passage, or transit, lets us measure the planet's size but not the shape of its path.

The globular cluster M22 is a dense swarm of hundreds of thousands of stars, hanging in our galaxy like a glowing beehive. In such a crowded environment, stars often collide and swap partners, but massive objects like black holes were thought to be quickly ejected by gravitational interactions.

When two galaxies collide, their central black holes begin a long dance of approach. Until they merge into one, we can see a pair of quasars — bright beacons that ignite as the black holes consume gas and dust. Such pairs in the sky are like two lighthouses standing close together, each shining from its own harbor.

Eclipses in binary stars are like clockwork: a white dwarf (the dense remnant of a star) regularly passes in front of its companion, and the light briefly dims. But for most such pairs, the clock runs fast or slow by seconds over years. Astronomers measured these glitches in 43 systems and found a pattern.

For 39 years, astronomers have been recording how the star BE Lyn brightens and dims. Its light pulsates with a rhythm of several hours, like a lighthouse that never stops blinking. But there is a glitch in this rhythm: sometimes the flashes came a little early, sometimes a little late. The star was moving closer to Earth and then farther away, as if something were dragging it in a circle.

Two stars, drawing together in a cosmic dance, experience an extra wobble — a consequence of spacetime curvature (an effect predicted by Einstein). A planet orbiting them also wobbles. Sometimes the rhythms align: the gravitational tugs from the stars fall in step with the planet’s orbit, like hands pushing a swing.