Why Not Even Light Can Escape a Black Hole: Gravity, Spacetime and the Event Horizon Explained

Light travels at 299,792 kilometres per second. Nothing in the known universe moves faster. Yet a black hole stops it dead, not by slowing it down, but by curving the space it travels through until every possible path leads inward. That is the key shift: a black hole does not grab light the way a hand grabs a ball. It restructures the geometry of spacetime itself.
In ordinary space, light moves in straight lines. But spacetime is not a fixed stage, it bends in the presence of mass, as Albert Einstein described in his 1915 general theory of relativity. Near a black hole, that bending becomes so extreme that the straight-line path light naturally follows curves back toward the centre. The light is not being pulled. It is simply going straight through a space that has been folded inward.
The event horizon is the boundary where escape becomes geometrically impossible. Cross it and the singularity at the centre is not just in one direction, it is in every direction, including what was previously called "the future." Spacetime inside the event horizon is oriented so that all paths through it, every trajectory any object or photon can take, lead toward the singularity. There is no sideways. There is no back. There is only in.
The radius of the event horizon for a non-rotating black hole is called the Schwarzschild radius, named after the German physicist Karl Schwarzschild, who derived it in 1916 while serving on the Eastern Front during the First World War. For an object with the mass of the Sun, this radius is about 3 kilometres. The Sun itself is roughly 696,000 kilometres in radius, meaning you would have to compress the entire Sun into a sphere smaller than a typical Indian city's metro station to create a black hole from it. Earth's Schwarzschild radius is about 9 millimetres.

The most common route is stellar collapse. A massive star, typically more than 20 times the mass of the Sun, burns through its nuclear fuel over millions of years. While fusion is active, the outward pressure of energy balances the inward pull of gravity. When the fuel runs out, that balance collapses. The core implodes in milliseconds. If the remaining mass is dense enough, no known force can halt the collapse, and a singularity forms: a point where density becomes, mathematically, infinite and the known laws of physics stop giving useful answers.
There are also supermassive black holes, which sit at the centres of most large galaxies, including our own Milky Way. The one at the centre of the Milky Way is called Sagittarius A* and has a mass of about 4 million Suns. In 2022, the Event Horizon Telescope collaboration released the first direct image of Sagittarius A*, showing the bright ring of superheated gas orbiting just outside its event horizon. The black hole itself appears dark, not because it is empty, but because no light from that region reaches us.

India's engagement with high-energy astrophysics, the field that studies black holes through X-ray and gamma-ray observations, has grown substantially through ISRO's AstroSat mission, launched from Sriharikota in September 2015. AstroSat is India's first dedicated multi-wavelength space observatory and has observed X-ray binaries, systems where a black hole or neutron star strips matter from a companion star. That infalling matter heats to millions of degrees and emits X-rays just before crossing the event horizon. AstroSat cannot see inside a black hole, but it reads the signature of matter at the edge, which is the closest any instrument can get.
India's scientific community also contributed to the broader global effort through researchers involved in the LIGO-India collaboration. Gravitational waves, ripples in spacetime first directly detected by the LIGO observatories in the United States in 2015, are produced when two black holes spiral into each other and merge. The planned LIGO-India detector in Maharashtra will add a third node to the global network, improving the precision with which scientists can locate the source of these mergers in the sky.General relativity predicts the singularity but cannot describe it. A point of infinite density is a signal that the theory has hit its own boundary. Physicists broadly agree that a complete theory of quantum gravity, one that merges general relativity with quantum mechanics, would replace the singularity with something finite and describable. String theory, loop quantum gravity, and other frameworks attempt this, but none has been confirmed experimentally.

Stephen Hawking showed in 1974 that black holes are not entirely silent. Quantum effects near the event horizon cause them to emit radiation, now called Hawking radiation, at an extremely low temperature. For a stellar-mass black hole, this temperature is far below even the cosmic microwave background, making it undetectable with current instruments. Over an almost incomprehensibly long period, a black hole losing energy this way would eventually evaporate entirely. What happens to the information about everything that fell in is one of the deepest unsolved problems in theoretical physics.
The reason light cannot escape a black hole and the reason a singularity cannot be described by current physics are the same reason: both sit at the place where gravity has won so completely that the ordinary rules no longer hold. The event horizon is not a wall, it is the last line where the geometry of spacetime still permits the concept of escape to mean anything at all.