Joe Scalone @ScaloneJoe

🌞That is how the Sun's gravity holds the planets together.

The three-body problem broke Newton, broke Poincaré (who ended up inventing chaos theory trying), and was finally cracked open by Chenciner & Montgomery in 2000: the figure-8 in clip 4 is their proof. Šuvakov & Dmitrašinović added 13 more families by 2013. Every clip is a real numerical integration of F = G·m₁m₂/r² with equal masses, no fudging. Math from 1687 still has surprises in it. [🎞️ extract: From Infinity with Love]

Güneşin yerçekimi gezegenleri işte böyle bir arada tutuyor.

Fundamental Mechanical Engineering Formulas.

Billionaire's WARNING: I'm SELLING. The Crash Is Already Here! youtu.be/32u5T6lO8qk?si… via @YouTube

Chinese AI systems have matched the performance of Anthropic’s powerful model Mythos in some cybersecurity scenarios, a development poised to reset the global tech race wsj.com/tech/ai/chines… via @WSJ

The thing that doesn’t fit is the thing that’s most interesting. -- R. Feynman

Neutron stars are often described as the corpses of massive stars, but that description almost makes them sound passive. In reality, they are among the most extreme laboratories in the universe: objects where gravity, nuclear physics, magnetic fields and relativity are pushed into regimes that no experiment on Earth can reproduce. A neutron star is born when a massive star exhausts its nuclear fuel and its core collapses under gravity. The outer layers are expelled in a supernova, while the inner core is compressed into an object only about the size of a city, but with more mass than the Sun. During that collapse, atoms are crushed so violently that electrons and protons are forced together, forming neutrons. The result is matter packed at a density comparable to, and possibly beyond, that inside an atomic nucleus. That is what makes neutron stars so scientifically valuable. They are not just astronomical objects; they are natural experiments in the behaviour of matter under almost impossible pressure. One of the central questions is what actually exists inside them. We know the outer layers contain neutron rich matter, but the deep interior remains uncertain. It may be a superfluid of neutrons, or it may contain more exotic states of matter: hyperons, Bose condensates, or even deconfined quark matter. In other words, a neutron star may contain forms of matter that have not existed freely since the earliest moments of the universe. This is why studying their mass and radius is so important. A slightly larger or smaller radius is not a minor detail; it changes what kinds of matter can survive inside. If a neutron star is very compact, the matter inside must be highly compressible. If it is larger, the internal pressure must be stronger. These measurements help constrain the equation of state, the physical relationship between pressure, density and temperature inside nuclear matter. It is one of the great unsolved problems connecting astrophysics with particle physics. Neutron stars also allow us to test gravity in one of its strongest forms. Their surfaces have gravitational fields billions of times stronger than Earth’s. Light escaping from them is bent and redshifted by the curvature of spacetime. In binary systems, especially when two neutron stars orbit each other, their motion becomes a precise probe of general relativity. When they finally merge, they release gravitational waves: ripples in spacetime that carry information about their masses, spins and internal structure. The merger of two neutron stars is especially important because it links several branches of astrophysics at once. It produces gravitational waves, electromagnetic radiation, gamma ray bursts, kilonovae and heavy elements. Many of the elements heavier than iron, including gold, platinum and rare earth elements, are thought to be forged in these violent collisions through rapid neutron capture. That means neutron stars are not only remnants of dead stars; they are also cosmic factories that help seed galaxies with some of the most valuable and complex elements in nature. Some neutron stars become pulsars. These objects emit beams of radiation from their magnetic poles, and as the star rotates, those beams sweep across space like a lighthouse. When one points toward Earth, we see regular pulses. Some pulsars are so stable that they rival atomic clocks. This makes them powerful tools for testing physics, mapping the interstellar medium and searching for subtle effects such as low frequency gravitational waves. Others become magnetars, a rare and even more extreme class of neutron star with magnetic fields trillions of times stronger than Earth’s. Their magnetic energy can crack the crust, trigger starquakes and release enormous bursts of X rays and gamma rays. A magnetar is a reminder that a neutron star is not simply a dense ball of matter; it is a dynamic object where magnetic stress, crustal physics and relativistic plasma can interact violently. What makes neutron stars so compelling is that they sit at the boundary between what we understand and what we can only infer. They are small enough to seem almost unreal, yet massive enough to warp spacetime dramatically. They are dead stars, but they can pulse, flare, collide and manufacture heavy elements. They are astronomical objects, but their deepest importance may lie in what they reveal about matter itself. Ultimately, the study of neutron stars matters because it does not only ask what these objects are. It asks what matter becomes when gravity has compressed it almost to the limit, how spacetime behaves around ultra compact objects, and how the universe builds some of its heaviest elements. Neutron stars are not just remnants. They are physical extremes made visible.

Einstein's General Theory of Relativity transformed our understanding of gravity, space and time. More than a century later, many of its predictions have been confirmed through observations, while others remain fascinating possibilities that scientists continue to investigate. Proven: -Gravitational lensing -Gravitational waves -Time dilation -Black holes Still unconfirmed: -White holes -Wormholes Some of Einstein's boldest ideas turned into scientific reality while others are still waiting for evidence. Which prediction do you think will be confirmed next?

Evolutionary Roots of Laughter Shared Between Humans and Great Apes, Study Finds ground.news/article/great-… #groundnews via @Ground_app

“Logic will get you from A to Z; imagination will get you everywhere.” — Albert Einstein

Gravitational time dilation is one of the most remarkable predictions of Einstein’s general relativity. A clock closer to a massive object ticks more slowly than one farther away, described by T = T′√(1 − 2GM/rc²) The effect is tiny on Earth but becomes dramatic near neutron stars and black holes. Time is not the same everywhere in the universe. It depends on where you are in a gravitational field.

"What we observe as material bodies and forces are nothing but shapes and variations in the structure of space and time." – Erwin Schrödinger

🚨: Time doesn't exist everywhere and it might not exist forever, new theory indicates

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🌟Find out more about the discovery, including videos & images, at: chandra.si.edu/photo/2026/m83/

NASA @NASA

a week ago

Sparkly, swirly, and surprising 🌌 @chandraxray data shows that this galaxy, Messier 83, is unusual. Over 20 of its supernova remnants – remains from star explosions – vary drastically in X-ray brightness. Typically, the remnants' brightness would fade slowly over time.

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✨ Map of the Universe: Look 11 Billion Years Back Scientists have unveiled a stunning map of the Universe, created using redshift data from distant galaxies and quasars. This image is a true time capsule, showing what our cosmic home looked like at a distance of up to 11 billion light-years from us.

For the first time ever, plasma inside the ST40 fusion reactor has been filmed in full color. Captured at 16,000 fps, this breakthrough lets scientists study plasma flow in stunning detail — a bright step toward clean fusion energy. [📹 TokamakEnergy]

The Carrington Event—the most powerful solar storm in history In 1859, Earth was hit by the most powerful geomagnetic storm ever recorded. It was called the Carrington Event. It was caused by a coronal mass ejection (CME). A cloud of solar plasma reached the planet in just 17.6 hours, compared to a typical 2-3 days. The storm caused bright auroras, telegraph failures, electric shocks to operators, and fires at stations. If such a storm were to occur today, satellites, communications, and internet would be damaged.

Mathematics and mystery. Shiver in ecstasy. The circle that fits precisely inside a 3-4-5 Pythagorean triangle has an area of π. OMG.

🌀 Milky Way is traveling through space at 600 kilometers per second, oscillating slightly, as if it were flapping its wings through the cosmos.