Black Holes Are Not What We Thought | Webb's New Discovery

How long does it take a black hole to grow a billion solar masses? You might expect a process on that scale to take an enormous amount of time, yet these giants already existed when the universe was only a few hundred million years old. They outshine some galaxies, and their light reaches us across billions of light years. What allowed them to gain mass so quickly? Could some of them have been massive from birth? And what new type of object did the James Webb Space Telescope discover just recently? You'll find out all of this and more in this episode. Hey, I'm Justin, and this is a new format here on Cosmo. Here, I break down the most complex ideas about space and the universe in clear, simple terms. I also cover new discoveries that let us see even familiar phenomena in a brand new light. And today, we're talking about black holes. To understand where the first supermassive black holes came from, we need to look back to the era when they were only beginning to grow. To do that, astronomers searched for their possible precursors, less massive objects that are still growing. Light from distant galaxies takes billions of years to reach us, so the James Webb Space Telescope lets us see them as they were in the distant past. The most valuable discoveries show us what surrounded a young black hole and what kind of material it was consuming. In August 2026, a team of astronomers from the Massachusetts Institute of Technology and other research centers reported their findings on an object called mom black hole star 1. We see it as when the universe was only 660 million years old. Its light took more than 13 billion years to reach us. In the images, it's a tiny red dot, yet its estimated luminosity is around 80 billion times that of the sun. What's more, its spectrum contains a dip that resembles the signature of light absorption in a stellar atmosphere, but the dip is so deep that ordinary starlight cannot account for it. To understand this phenomenon, the scientists calculated what a black hole concealed within an extremely dense envelope of gas would look like. Radiation produced near the black hole cannot escape freely. The gas absorbs it and then re-emits it in an altered form. As a result, the black hole itself remains hidden, while the gas envelope around it shines so brightly that, from a distance, the entire system resembles an enormous star. The model reproduced the key features of the observed spectrum. After considering the possible explanations, the astrophysicists concluded that the object represents an entirely new class of cosmic object, a black hole star or quasi-star. Put simply, it's a supermassive black hole surrounded by a dense, extremely hot envelope of gas, much like an ordinary star. In this configuration, the central black hole has a mass of about 10 million solar masses. The surrounding gas glows because matter falling inward heats up, not because of nuclear fusion. For the first time, astronomers have an object that they can use to test what a black hole hidden inside a dense gas envelope might actually look like. In fact, Mom Black Hole Star 1 is not the only strange object spotted in the young universe. In July 2026, for example, researchers reported 31 new distant quasars discovered in data from the Euclid Space Telescope. We see them as they were when the universe was less than a billion years old. Earlier still, the James Webb Telescope discovered more than 200 so-called little red dots, mysterious objects that may resemble quasi-stars. It's not so easy to explain how such giants emerged within the first 200 billion years. If a black hole starts out at only a few dozen solar masses, it must grow many times over. The amount of surrounding material matters, but so does the rate at which the black hole can accrete it. To understand whether a dense gas envelope could speed up this process, let's take a closer look the black hole itself and at what helps it gain mass and what gets in the way. A black hole is a region of space-time from which nothing, not even light, can escape. Its boundary is called the event horizon. Any matter or radiation that crosses it can never return. Black holes are generally surrounded by a massive rotating disk of gas and dust called an accretion disk. Gravity accelerates the material in the disk, causing it to glow brightly. Most known black holes were detected through radiation from their accretion disks. Black holes are generally divided into three main groups by mass. Stellar mass, intermediate mass, and supermassive. In practice, mass is simply the easiest property to measure. The real difference lies in how they're formed. Stellar mass black holes generally form at the end of the life cycle of massive stars. Once a star exhausts its nuclear fuel, it explodes in a supernova, and the resulting shockwave compresses its core into an ultra-compact object, a black hole. Their masses are generally tens of solar masses and rarely exceed 100, while their radii are only a few dozen kilometers. The supermassive black holes can be found at the centers of large galaxies, including our own. They are millions or even billions of times more massive than the Sun. For example, Sagittarius at the center of the Milky Way has a mass of about 4 million solar masses. It is currently thought that supermassive black holes formed in the early universe through the gravitational collapse of giant clouds of gas and dust. Between these groups lie intermediate mass black holes, ranging from hundreds to tens of thousands of solar masses. They are extremely rare and mysterious celestial objects, with only a few hundred candidates identified so far. One possible example lies at the center of the star cluster, Omega Centauri. Calculations suggest that it has a mass of about 8,200 solar masses, although the black hole itself cannot be observed directly. In addition to the three main groups, scientists also consider hypothetical types of black holes. Among the most interesting are primordial black holes. These objects may have formed in the first moments after the Big Bang, long before stars appeared. If a region of the young universe was significantly denser than the surrounding space, its own gravity could have compressed the matter into a black hole. Now, unlike ordinary black holes, these would not require the death of a star. That means their possible mass range is much broader. Some primordial black holes could have been tiny while others could have been comparable in mass to stars or far heavier. The lightest of them should have vanished by now, while more massive ones may, in theory, have survived to the present day. That is why primordial black holes are considered possible candidates for dark matter. They emit no light of their own, but they do exert a gravitational pull and can affect the motion of ordinary matter. Another hypothetical type is the microscopic black hole. Here the name refers not to its origin but to its extremely small size. Some theories suggest that such objects could have formed in the early universe or even been created in collisions between particles at enormous energies. Scientists have searched for their signatures at the Large Hadron Collider but none have been found so far. According to Stephen Hawking's calculations, black holes should emit particles and gradually lose mass. The smaller a black hole is, the higher its temperature and the faster it evaporates. A microscopic object created in a particle collision would therefore exist only for a tiny fraction of a second. We would not be able to see the black hole itself, but detectors could register the stream of particles produced as it evaporated. Those are the signals scientists are trying to detect. Whatever the origin, early black holes had to gain an enormous amount of mass in a short time. But why is it that difficult even when they're surrounded by plenty of material? A black hole can grow in two main ways, by accreting matter from its surroundings and by merging with other black holes. Sustained growth requires a steady supply of material that actually reaches the black hole. However, some of that material remains in the rotating disk or is ejected back into the surrounding space. So even an abundance of gas in a galaxy does not necessarily mean that a black hole can gain mass quickly. There is another obstacle that limits how quickly a black hole can grow. Matter falling toward it gradually heats up and releases energy as radiation. That radiation, in turn, pushes against the surrounding gas and prevents it from moving farther toward the center. The hotter the material around the black hole becomes, the greater the outward radiation pressure. certain point, that pressure balances the gravitational pull, and this theoretical threshold is called the Eddington limit. This limit helps estimate how quickly a black hole can grow under ordinary conditions. In some environments, however, that limit can be exceeded, and the early universe may have provided just such conditions. This brings us back to the unusual object discovered by Webb. Its dense envelope may have altered the light escaping from it while also creating conditions that accelerated the black hole's growth. To see how, let's look at quasi-stars. A quasi-star is a theoretical object in which a black hole is hidden inside an enormous envelope of gas. From the outside, such a system might resemble a giant star, but instead of a conventional nuclear fusion energy source at its center, it contains a black hole that gradually accretes matter from its own envelope. As matter approaches the black hole, it heats up and releases energy. The surrounding gas envelope absorbs that energy and carries it to the surface, where it is radiated into space. This creates a layered system. The black hole accretes matter while the envelope redistributes the energy and makes the entire quasi-star shine. At the same time, energy moves outward not only through radiation. The gas inside the envelope is constantly circulating. Hotter layers rise towards the surface while cooler layers move towards the center. A similar process occurs inside ordinary stars. It helps transport energy from the interior towards the surface. But why does this envelope help the black hole grow instead of flying apart under radiation pressure? Well, the answer lies in its mass. In the classical quasi-star model, the envelope is far more massive than the black hole itself. Its own gravity holds the gas together, allowing the system to remain stable even with an extremely powerful energy source at its core. The envelope's gravity therefore allows the black hole at the center of a quasi-star to accrete more matter over the same period, and grow much faster than an equally massive black hole without such an envelope. But the system gradually changes. The central black hole gains mass, the envelope expands, and its surface cools. In this classical model, the envelope eventually becomes unstable and disperses. What remains is a black hole that has grown substantially over the lifetime of the gas envelope. That is why these objects interest astronomers. They may have allowed the first black holes to gain mass rapidly and then continue growing after the envelope dispersed. But rapid growth is only part of the story. The mass a black hole started with matters too. Could some black holes have been born massive? The direct collapse model explores that possibility. Direct collapse means that an enormous cloud of gas contracts under its own gravity, bringing most of its matter together at the center. This gives rise to a super giant star and then, even after more intense compression, to a super massive black hole. this scenario requires special conditions. Normally, the cloud fragments into separate clumps that form many stars. The material is divided among them instead of collecting into one enormous object. So what could keep the cloud from breaking apart? Temperature plays a crucial role. As long as the gas remains hot, its pressure prevents individual regions of the cloud from contracting. Molecular hydrogen, however, acts as a coolant, allowing some of the cloud's energy to escape as high-energy photons. For more material to collect at the center, their cooling must be limited. Ultraviolet radiation from nearby young stars can help. It destroys molecular hydrogen and slows the cooling. Under the right conditions, this keeps the cloud from breaking into many clumps and directs more material towards the center. But the right conditions do not arise everywhere. Nearby stars must produce enough ultraviolet radiation to suppress the cloud's cooling. Researchers are therefore looking for other possible sources of this radiation. One of the most unexpected possibilities involves dark matter. In a 2024 paper, scientists at the University of California Los Angeles considered the possibility that some dark matter particles could decay and emit photons. This radiation could inhibit the buildup of molecular hydrogen and prevent the cloud from cooling rapidly. More material could then collect in a single massive object instead of being distributed among many stars. According to the authors' calculations, dark matter particles with the right properties could indeed create the conditions for a massive black hole to form, and the necessary radiation would be produced inside of the cloud itself. Another possibility is that a black hole could have gained a significant share of its mass during brief but extremely intense periods of growth. In a 2026 paper, researchers examined how such episodes could occur in the centers of young galaxies. Mergers and close encounters between young galaxies could channel enormous volumes of gas toward their centers. This could create a dense region where stars formed while a black hole grew. The authors call this process a nuclear burst. This large-scale inflow of matter can be so powerful and rapid that light becomes trapped within it and it cannot escape. According to the calculations, this can allow black holes to accrete matter up to 10 times faster than under ordinary conditions. A single burst lasts less than a million years, but many such bursts can occur over the course of a galaxy's history. In the researcher's model, these episodes allow black holes to reach hundreds of thousands or even millions of solar masses. The compact red dots discovered by James Webb's space telescope may be systems caught in a brief phase of especially rapid black hole growth. During this phase, the black hole shines brightly enough to stand out against the surrounding stars, and the dots we can see may be only the brightest members of a far larger population that current telescopes cannot yet detect. All of this gives us a new way to view Mom Black Hole Star 1. In James Webb images, it is just a red dot, but its light gives us a glimpse of one of most fascinating stages in black hole evolution, a time when dense surrounding gas may have created the conditions for rapid growth. We still cannot say for certain that this object is a quasi-star, however the model of a black hole inside a dense gas envelope explains the object's unusual properties and gives astronomers a way to test what such a system might actually look like. The first cosmic giants, however, may not all have followed the same path. Some black holes may have been born massive, while others may have grown thanks to an abundant supply of material. And some may have passed through several of these stages. The central question now is what role each of these processes played in the early universe. With new observations from Webb, astronomers can search for the answers by studying individual objects whose light took more than 13 billion years to reach us. Alright guys, we worked really hard on this episode and we'd love to hear what you think. Tell us in the comments below what stood out to you, and also what discoveries would you like to hear about in future episodes of Cosmo Here. We want to make space accessible to everyone, and your support makes a real difference. Every like and comment helps bring the universe a little closer, and makes it easier to understand, for me and for you. So, I'm Justin, and I'll see you next time.