Gravity will not stop. As far as physics can tell us, gravity is a fundamental feature of the universe that persists as long as mass, energy, or even curved spacetime exists. There is no known mechanism, no timer, and no theoretical prediction that gravity will one day switch off. But the story is more nuanced than a simple “no,” because the universe’s expansion is already weakening gravity’s practical reach in ways that matter over cosmic timescales.
Why Gravity Cannot Simply Turn Off
Gravity is not a fuel that gets spent. In general relativity, Einstein’s theory that has held up for over a century, gravity is the result of mass and energy curving the fabric of spacetime. Objects follow that curvature, which we experience as gravitational attraction. As long as there is mass or energy anywhere in the universe, spacetime will curve around it, and gravity will operate.
Even in the absence of matter, the equations of general relativity allow for curved spacetime on its own. A physicist named Willem de Sitter showed this as early as 1916: empty spacetime can still be curved. Gravity feels strongest where spacetime is most curved and vanishes only where spacetime is perfectly flat. A perfectly flat, perfectly empty universe is a mathematical possibility, not a physical prediction for our cosmos.
What Dark Energy Does to Gravity’s Reach
Gravity won’t stop, but its ability to hold distant objects together is already losing ground. The universe’s expansion has been accelerating for roughly the last 5 billion years, driven by something physicists call dark energy. This mysterious component makes up about 70 to 75 percent of the universe’s total energy density, and it acts as a kind of cosmic repulsion, pushing space apart faster than gravity can pull things together at large scales.
The expansion rate, known as the Hubble constant, currently sits somewhere between 67 and 73 kilometers per second per megaparsec, depending on the measurement method. That disagreement is one of the biggest open questions in cosmology, but the range itself tells us something concrete: at enormous distances, space is stretching fast enough to carry galaxies away from each other despite gravity’s pull.
Over small scales, gravity wins easily. Our Local Group of galaxies, including the Milky Way and Andromeda, is held together by mutual gravitational attraction. The Milky Way even exerts a gravitational tug on a galaxy called NGC 3370, nearly 100 million light-years away. But that pull is so tiny at such a distance that the universe’s expansion overcomes it. The practical boundary where expansion beats gravity falls somewhere around the scale of galaxy clusters. Anything bound more tightly than that stays together. Anything farther apart drifts away, and that drift is accelerating.
If dark energy continues at its current strength, the long-term result is a universe that grows ever colder, ever emptier, and ever darker. The visible horizon around each observer would gradually shrink, leaving isolated pockets of gravitationally bound matter surrounded by unreachable void. Gravity would still operate within those pockets, but its influence across the wider universe would become effectively irrelevant.
The Far Future: What Happens to the Last Objects
Even in this increasingly sparse universe, gravity keeps working on whatever matter remains. Stars burn out. Galaxies within gravitationally bound groups merge. Eventually the only large gravitational sources left would be black holes, and even they are not permanent. Through a process called Hawking radiation, black holes slowly lose mass by emitting tiny amounts of energy. The rate is extraordinarily slow. A black hole with the mass of our sun would take roughly 10 to the power of 71 seconds to evaporate, a number so large it dwarfs the current age of the universe by a factor beyond comprehension. Supermassive black holes, billions of times heavier, would last proportionally longer.
Once a black hole fully evaporates, its gravitational field goes with it, because the mass that produced it is gone. But that is not gravity “stopping.” That is mass converting into radiation, which itself still has energy and still curves spacetime, just spread so thin it becomes negligible. Gravity as a force remains intact. It simply has less and less concentrated matter to work with.
Could Gravity Weaken at Extreme Scales?
Some approaches to quantum gravity, the effort to reconcile gravity with quantum mechanics, have produced interesting hints. One version called quadratic gravity found that when gravitons (the hypothetical particles that would carry the gravitational force) collide at extreme energies, gravity actually gets weaker rather than stronger. Physicists call this asymptotic freedom, and it suggests that gravity may behave differently at the tiniest possible scales. But “differently” does not mean “disappears.” The researchers involved describe the result as pointing toward spacetime continuing forever, a true description of reality all the way down to arbitrarily small scales.
No major theory of quantum gravity predicts that the gravitational force will decay over time or eventually cease to exist. The open questions are about how gravity behaves under extreme conditions, not whether it has an expiration date.
What This Means in Practical Terms
Gravity keeps you on the ground, keeps the Earth orbiting the Sun, and keeps galaxies clustered together. None of that is going away on any timescale relevant to human life, or even to the life of stars. The Sun will burn out in about 5 billion years, and gravity will still be pulling on whatever remains.
The scenario where gravity “loses” is not one where the force itself disappears. It is one where the universe expands so much that matter becomes too spread out for gravity to connect distant objects. Locally, within bound systems like solar systems, galaxies, and galaxy clusters, gravity continues to dominate. The force itself is as permanent as anything physics has identified. What changes over cosmic time is not gravity’s existence but the landscape of matter it has to work with.