Webb

James Webb has had to investigate whether he was born “from the top down” or “from the bottom up”

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29 Cygni b is a huge celestial object, with a mass equal to 15 times the mass of Jupiter. Apparently it is a planet, but that mass could place it as a star. For example, a brown dwarf. Therefore, a team of astronomers has used the James Webb to analyze its origin, further refining the concept of the formation of stars and planets. A question of metals. The authors of the study, who it was just publishedhave used the NIRCam camera on the James Webb Space Telescope to take photographs of this planet. This instrument allows high-resolution images and spectroscopy measurements to be taken, with which the composition of the atmospheres of stars and planets can be studied, taking into account how they reflect light. Thanks to this, it has been seen that 29 Cygni b is very enriched in metals compared to the star around which it is located. Specifically, it has an amount of metals equivalent to 150 Earths. This is compatible with the accretion of a large amount of metal-laden solids into a protoplanetary disk. It is then confirmed that it is a planet, but a planet very unusual. Planet or star? That’s the question. Planet formation takes place in a bottom-up process. In a disk of gas and dust, known as a protoplanetary disk, dust particles collide to form small fragments of rock and ice, which continue to clump together and grow until they form a planet. It is a process called accretion. The largest ones, in addition, in this process capture gas, which is why they later become gas giants. On the other hand, stars form from top to bottom. A gas cloud fragments and each fragment collapses under its own gravity, becoming smaller and denser. From paradox to paradox. This definition could lead us to think that planets are larger than stars. After all, planets go from less to more and stars from more to less. However, that is not true. Stars form when huge clouds of gas collapse, so they are still very massive. So much so that nuclear fusion can occur in them due to the high conditions of pressure and temperature. On the planets, although there is a growth from less to more, it is not so great. The problem is that with planets as immense as 29 Cygni b there are doubts about the formation from less to more. It would seem that they were also formed by a fragmentation process in protoplanetary disks. As explained by the European Space Agency in a statementis something that “could explain why some very massive objects are found billions of kilometers from their host stars, in regions where the protoplanetary disk should have been too weak for accretion to occur.” That’s just what happens with 29 Cyni b. It has an enormous mass and is 2,400 kilometers from its star. What James Webb teaches us. The fact that 29 Cygni b is so rich in metals indicates that it must have been formed by an accretion process, in which it accumulated more and more. In fact, heIt is normal for a planet to have many metals in proportion to its starwhich happens in the system in which 29 Cygni b is located. In short, it is shown that much larger planets than we thought can be formed by accretion, without having to resort to a top-down process. And now what? 29 Cygni b has been the first of the four objects that will be studied by James Webb. All of them have a mass between 1 and 15 times that of Jupiter and are at least 1.5 billion kilometers from their star. This indicates that they are all in that dilemma of being huge planets or another star. Cataloging them into one of the two groups can help us understand much better the process by which the largest planets are formed. Image | NASA, ESA, CSA, J. Olmsted (STScI) In Xataka | Since we were children we have been told that Jupiter is enormous, colossal, exaggeratedly large. It is 8 km smaller and that changes everything

James Webb has bad news for the largest natural laboratory for rocky planets, but there is still some hope

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The star TRAPPIST-1 and the seven known planets that surround it are a natural laboratory in which the evolution of rocky planets can be studied. This has led many scientists to focus their attention on them, in search of a possible habitable planet. However, observations made by an international team of astronomers with the help of the James Webb Space Telescope They are not very encouraging. Planets without atmosphere. The James Webb Space Telescope has a very powerful infrared radiation analysis instrument, with which it can analyze the temperature of the planets it observes. These emit infrared radiation whose intensity is proportional to their temperature, so a thermal map can be made. That’s what these astronomers have done. They have initially focused on two of the planets that orbit TRAPPIST-1: TRAPPIST-1a and TRAPPIST-1b. The resulting heat map shows that neither planet has an atmosphere. They may have had it one day, but possibly TRAPPIST-1 itself destroyed it. It is a very uninspiring result for the search for habitable planets in this system. Lights and shadows of TRAPPIST-1. So far seven exoplanets have been discovered orbiting TRAPPIST-1. They are all very close together. In fact, its seven orbits are concentrated in the distance between Mercury and the Sun. What happens is that this red dwarf is less energetic than our Sun, so the temperature would not be as suffocating. All of these planets are rocky, like Earth, and in fact, some are very similar in size. There could be an exoplanet with conditions similar to ours. The problem is that red dwarfs They emit a lot of radiation and energetic flows of particles that could destroy their atmosphere.. And of course, without atmosphere, there is no life. Tidal lock. All planets in the TRAPPIST-1 system are tidally locked. This means that its rotation and translation period around the red dwarf they are synchronized. As a result, there is one side continuously exposed to the star and another on the opposite side. On one side it is always day and on the other it is always night. NASA/JPL-Caltech Extreme temperatures. When a planet is tidally locked, there can be two situations, depending on whether it has an atmosphere or not. When there is an atmosphere, heat flows from the light side to the dark side, so that the entire planet has a stable average temperature. On the other hand, if there is no atmosphere, the dark side can be frozen and the illuminated side can be scorched. In the two exoplanets analyzed by James Webb, it has been seen that temperatures are around 100ºC-200ºC on the illuminated side and -200ºC on the dark side. Therefore, it is confirmed that there is no atmosphere. And now what? Despite this hard blow, there is still hope. The two exoplanets that have been analyzed are not in the star’s habitable zone. This is the distance from it at which the temperature is adequate for the water, if any, to remain in a liquid state. At that exact point there are only TRAPPIST-1e, TRAPPIST-1f and TRAPPIST-1g. Furthermore, the former has a density and size very similar to those of Earth. James Webb has all his attention on this exoplanet right now, to repeat the process. If there were an atmosphere on it, it could still remain on the list of possible habitable planets. It’s still interesting. Despite the first blow, TRAPPIST-1 remains a very interesting system for understand the evolution of rocky planets. The Earth was lucky not to lose its atmosphere; but, beyond those, the evolutions can be similar. Furthermore, we have not yet ruled out that TRAPPIST-1e has an atmosphere. Let’s go step by step. Image | NASA, ESA, CSA, Joseph Olmsted (STScI) In Xataka | There is only one chance in 11,000 years to reach the planet Sedna. Some Italians want to use this nuclear engine

The James Webb Telescope has finally discovered Saturn’s best kept secret

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Saturn has become a headache for scientists since the Cassini probe in 2004 took action of its rotation speed that did not coincide with the figures accepted in the scientific community. Little by little, new data has been discovered that helps explain this inconsistency, but it has been necessary for the James Webb Space Telescope to come into play to find the definitive answer. Cassini’s incoherence. In 2004, the Cassini probe took advantage of its visit to Saturn to measure some important dataas its rotation speed. Normally this is calculated by analyzing parameters that occur periodically, such as radio emission pulses. It is a very consolidated method, which has been used to calculate the rotation rate of many planets. With Cassini, it was expected to obtain a figure that would coincide with what the Voyager 2 probe had previously taken in 1981. However, to the surprise of the scientists who studied the data, the numbers didn’t add up. A mysterious push. A planet cannot speed up or slow down without an external force driving it. There should be something driving those changes in rotation speed. Or, at the very least, some unknown factor that was falsifying the results. All this was a mystery until 2021, when a team of scientists from the University of Leicester published a study in which new clues were provided. The auroras enter the scene. For a month, scientists at the University of Leicester measured infrared emissions in Saturn’s upper atmosphere. This allowed them to map a series of variable fluxes of activity in the ionosphere, the layer of the atmosphere in which ionized particles are abundant. That is, atoms that have gained or lost electrons and have acquired a negative or positive charge, respectively. These flows were related to the formation of auroras. However, there was something strange. Unlike on other planets, including Earth, a good part of these auroras were produced by the action of rotating winds within Saturn’s own atmosphere, not only by the influence of the magnetosphere. A reminder about the auroras. The auroras are formed when charged particles interact with the atoms that make up a planet’s atmosphere, exciting them and causing the emission of light. Normally, these charged particles come from solar activity, as happens on Earth, or from volcanic eruptions on nearby moons, as happens on Jupiter. Be that as it may, they are concentrated in a region external to the planets, known as the magnetosphere. In the case of Saturn, the 2021 study showed that auroras were also forming within the planet’s own atmosphere. On Earth, auroras are formed by solar activity A puzzle still incomplete. The interaction of molecules and atoms in the atmosphere with charged particles does not only cause the emission of light. It also causes the emission of radiation in other regions of the spectrum. For example, radio pulses. Let us remember that these pulses are the ones that were used to measure the rotation of Saturn. The auroras could be falsifying them. These auroras, as we have seen so far, are produced by the action of rotating winds in Saturn’s own atmosphere. But where do those winds come from? The rock star arrives. The James Webb Space Telescope is the rock star of space telescopes. A state-of-the-art instrument, capable of reaching where other telescopes could not. Therefore, thanks to him, the necessary measurements could be taken to find the origin of Saturn’s winds. Specifically, it has captured the glow caused in the infrared by a molecule in Saturn’s upper atmosphere, called trihydrogen cation. This is very useful, because it acts as a kind of thermometer. It is very susceptible to environmental conditions, so its ionization state helps to know the surrounding temperature. By carefully analyzing its state in different regions of Saturn’s northern hemisphere, it has been possible to make a map of both temperatures and particle density. The missing piece. The temperature and particle density patterns match those predicted in a series of computer models 10 years ago. In these models, these patterns originated when the auroras themselves acted as a heat source. The endless cycle. What happens is this: the auroras, with all their display of light and radiation, heat the atmosphere at a specific point. This heating causes the movement of particles between points at different temperatures, generating a wind charged with electricity. This wind, in turn, propels electrically charged particles, which cause more auroras to form. It’s a vicious circle or, as the authors of the study explaina planetary heat pump. A perfect system that feeds itself. And, of course, the mysterious external factor that upset scientists trying to measure Saturn’s rotation. Image | NASA | Bruce Waters (Wikimedia Commons) | Vincent Guth (Unsplash) In Xataka | James Webb has been detecting red dots in the universe for years: the only problem is that we don’t know what they are

The chemical composition of galaxies has always been full of unknowns. James Webb has taken a huge step to solve it

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The James Webb Space Telescope sees where others can’t: its infrared vision pierces clouds of cosmic dust and reaches galaxies so far away that it took billions of years for its light to reach us. Looking far into space is, in that sense, looking back in time. However, what James Webb has seen in these galaxies differs from what was expected: these early galaxies seem to have too much nitrogen, much more than expected. Among the exotic possible explanations of science, hypotheses such as gigantic stars never seen before, black holes functioning as catalysts for galactic chemistry or large quantities of stars have passed. In fact, that was the topic of conversation in the middle of a phone call while Mexican astrophysicist José Eduardo Méndez-Delgado waited in line for the doctor. On the other end of the line, his colleague Karla Arellano-Córdova, who was in Edinburgh. In that informal talk they decided to change the prism: perhaps the problem was not the galaxies, but how we measure them. The discovery. The proposal from this international team is to analyze three light signals from the same oxygen ion to calculate temperature and density at the same time, without starting from one to calculate the other (the original source of error). The result: the gas was a hundred or a thousand times denser than was assumed in those galaxies. With that correction, the galaxies turned out to be richer in metals than they appeared and the excess nitrogen was drastically reduced. Why it is important. First, because the metallicity of a galaxy is directly related to its history: the more metals there are in its composition, the more stars have been born and died within it. Until now we were underestimating this figure, which made those early galaxies appear very different from our own and suggested a sharp and discontinuous evolution. Now they look more like what we know. But the elements essential for life, such as carbon, oxygen or nitrogen, did not exist when the universe was born: they were manufactured by the stars inside and expanded when they died. Hence the interest in knowing the chemistry of galaxies: it helps to understand when the universe had the necessary ingredients for life. With the wrong measurements, we don’t know if those ingredients were there earlier and in more places than we thought. Context. The standard method to know the composition of a distant galaxy is to analyze the spectral lines of its light based on the density of the gas and its temperature. The problem is that in these primitive galaxies the gas is much denser than expected, so its application as a thermometer works poorly. And from here on, everything failed. The nitrogen anomalies appeared in the first scientific data from the James Webb Space Telescope, as this either this. Since the results did not fit the models, the scientific community threw itself into trying to find explanations. This paper proposes to take a step back: before interpreting stellar physics, check that the measurements are correct. Besides, the Webb now allows it: simultaneously detects oxygen lines in the ultraviolet and in the optical in such distant galaxies. How they do it. In essence, the trick is choosing the right signals. One of the oxygen light lines, visible in ultraviolet, has a special property: it does not distort even if the gas is very dense, something that happened with the lines they were using previously. By combining it with two other signals from the same atom, the research team can calculate temperature and density at the same time, as if they were solving two simultaneous and independent equations. Using statistical simulations, the team found that the results were consistent with other independent measurements of the same galaxies. Yes, but. As the team explains in the work, their method corrects the density error, but not other possible errors that are equally important: the gas of these galaxies also has internal temperature variations, and that can bias the results in ways that this study does not resolve. Furthermore, the method only works well when all three light signals from oxygen are clearly detected. In three of the six galaxies analyzed this was not possible, and the results are less precise. Nitrogen remains a problem. The overabundances come almost entirely from a particular ion whose emission is extraordinarily sensitive to temperature: a variation of just ten percent in that parameter would reduce the calculated nitrogen by half. No one has yet measured that temperature directly. However, it points out a path to follow before looking for “exotic” explanations: verify that the measurement tools are up to par. In Xataka | For a time it was one of the asteroids most watched by astronomers: the Webb has just resolved a key doubt In Xataka | James Webb has been detecting red dots in the universe for years: the only problem is that we don’t know what they are Cover | Oleg Moroz

He has achieved it by combining James Webb and Hubble

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There are images that do not need context to impose themselves. Saturn is one of them. It is enough to see it to understand why it continues to be one of the great protagonists of the solar system: for its shape, for its rings and for that mixture of apparent simplicity and complexity that it hides. The same thing happens to many of us, we stop at any new photograph as if it were the first. And that is somewhat logical, because we do not always have the opportunity to observe it with a such a rich comparison between visible and infrared light nor to get closer, even through an image, to what really happens in its atmosphere. On this occasion, what NASA has shown It is not simply a new photograph, but a different way of observing the same planet. In a single comparative image (Click to download the image in high definition), the agency has put together an observation from Hubble taken on August 22, 2024 and another from James Webb captured on November 29 of the same year, 14 weeks apart. The result is a double view that seeks not so much to impress as to explain how what we see changes when we observe at different wavelengths. What are we really seeing in this image? If we stop at the image, the difference is obvious from the first moment. On the left, the James Webb shows a Saturn with darker, more contrasting tones, where the rings shine brightly because they are made of highly reflective water ice. On the right, Hubble offers a view much closer to how we would perceive it with the naked eye, with soft colors and more subtle bands. According to NASA, both telescopes are observing sunlight reflected by the clouds and mists of the planetbut each one does so in different ranges, which radically changes the information they provide. On the left, the image of Saturn captured by the James Webb Space Telescope; On the right, the one obtained by the Hubble Space Telescope: two views that reveal its active atmosphere, its moons and its bright rings Beyond the visual contrast, this comparison allows us to peek into what happens inside Saturn’s atmosphere. The agency explains that by combining both observations, scientists can study the planet at different altitudes, from the deepest clouds to the highest and most diffuse regions. In the Webb image, for example, a long-lasting jet stream known as a “ribbon wave” appears and also a persistent remnant of the great spring storm of 2010 to 2012. Hubble, for its part, provides continuity in monitoring the bands and the general evolution of the planet. At this point, it is worth clarifying something important: we are not looking at two photographs that reproduce Saturn in the same way. The difference is in how the light is collected and interpreted. Hubble works in the visible spectrum, the same one our eyes perceive, which is why its image is more familiar. James Webb, in this case, observes in the infrared, a radiation invisible to us which allows detecting clouds and compounds at different depths in the atmosphere. In order to display this data, scientists translate these signals into visible colors, and from there come the unnatural tones that appear in your image. If we move all this to a closer scene, the most reliable reference would be the Hubble image. That is the closest thing to how we would perceive Saturn, with soft tones, not very marked bands and bright but natural rings. But the interesting thing is not to choose between one or the other, but to understand what each look contributes. Webb’s allows us to go beyond the visible and detect processes that would otherwise remain hidden. And it is precisely in that combination where this image gains all its meaning. Images | POT In Xataka | Artemis II will take NASA to the Moon half a century later. He will do it with the help of the University of Seville

the Webb telescope has just clarified a key doubt

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There are asteroids that go almost unnoticed and others that force us to look at them much more carefully. 2024 YR4 belongs to that second group. When it was discovered at the end of 2024, the first calculations of its trajectory still had enough margin of error to contemplate a very small possibility of impact with Earth. That scenario was soon ruled out, but, as ESA explainsthe case remained under follow-up for a different reason: a doubt was left open about the Moon which was not resolved until new observations arrived. Impact risk. With data available since spring 2025, trajectory models indicated that the asteroid had about a 4% chance of hitting the Moon on December 22, 2032, an estimate that NASA placed at 4.3% in its previous calculations. It was not a high percentage, but it was significant enough for the teams dedicated to monitoring near-Earth objects to follow it with special attention. Furthermore, we are talking about an object of about 60 meters. How Webb came into play. To clear up that doubt, something more than the usual telescopes was needed. An international team of astronomers identified two very specific windows in February 2026 in which the James Webb Space Telescope could try to detect the asteroid, which at that time was just an extremely faint point millions of kilometers away. It involved using one of the most complex scientific instruments built to date to locate an almost invisible object and measure its position with the necessary precision to project its orbit almost seven years into the future. Key piece. The observations were made on February 18 and 26, 2026 with the camera NIRCam of the James Webb telescope. From these images, astronomers compared the position of the asteroid with that of the background stars, whose coordinates are known with great precision thanks to ESA’s Gaia mission. ESA adds a relevant detail to understand why this went ahead: the planning and analysis was coordinated with ESA’s Near-Earth Object Coordination Center, NASA’s Center for Near-Earth Object Studies and the Webb mission team. With this new data package, the orbital models were adjusted enough to close the mystery. James Webb analyzed the position of the asteroid in relation to the background stars The flyby distance. With the new calculations, monitoring teams can now estimate quite accurately what the asteroid’s passage through the lunar environment will be like. According to NASA, it will pass on December 22, 2032 about 21,000 kilometers from the surface of the Moon. That range is enough to eliminate the impact scenario that had been on the table for months. In other words, the object will continue on its way through the solar system without hitting either the Moon or Earth. Surveillance doesn’t stop. Programs such as ESA’s Space Security or NASA’s tracking systems continue to detect and analyze near-Earth objects to anticipate any possible future threats. The logic is simple: the sooner a potentially dangerous object is identified, the more room there will be to study its trajectory and assess the real risk. In this case, the result has been reassuring, but it also illustrates, as ESA insists, what planetary defense means in practice when a doubt is resolved with more data and better measurements. Images | THAT In Xataka | We have been burning space junk for years to get rid of the problem. It turned out to be a bad idea

James Webb has opened the door to a fascinating world

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Until not so long ago, the word “exoplanet” seemed more typical of speculation than astronomy. Isaac Newton already dropped in the ‘Scholium Generale‘ of the Principia Mathematica that fixed stars could be the center of systems similar to ours, but science needed centuries to prove it. It was not until the late 1980s that the first signs of planets outside the Solar Systemalthough we had to wait until 1992 to confirm for the first time the existence of worlds beyond the Sun, around the pulsar PSR B1257+12. In recent decades, the pace of discoveries has skyrocketed thanks to increasingly precise instruments, which have allowed us to locate worlds that are as strange as they are fascinating. The Kepler space telescopefor example, identified more than a decade ago Kepler-16ba planet with “two suns” reminiscent of Tatooine from Star Wars. Since then we have cataloged a huge variety of exoplanets, but now the James Webb telescope presents an especially striking find: a world of boiling lava that, to the surprise of astronomers, is colder than theoretical models predict. An extreme world that questions what we know With a radius approximately 1.4 times that of Earth, TOI-561b It is an extreme super-Earth that orbits a star located about 280 light years away, in the constellation Sextans. NASA describes it as the innermost planet of a system made up of four worlds, with an immediate peculiarity: it completes an orbit in less than eleven hours. Its proximity is so extreme, barely 0.01 astronomical units, that the daytime hemisphere must greatly exceed the melting point of rocks. Everything points to a planet trapped by its star in a tidal lock, with eternal day on one side and perpetual night on the other. One of the peculiarities that most puzzles researchers is the low density of TOI-561 b. Astronomer Johanna Teske, lead author of the study, explains that “it is not a super-puff, but it is less dense than one would expect with a composition similar to that of the Earth.” The team envisioned the planet having a small iron core and a mantle made up of less compact minerals, a possibility that would fit the chemistry of its star. As it is a very old G-type star, about 10 billion years old and poor in iron, located in the thick disk of the Milky Way, it is plausible that the planet emerged in a primordial environment different from that of the Solar System. Still, the exotic composition did not resolve all the unknowns, and the team began to consider another possibility: that TOI-561 b was involved through a thick atmosphere. The idea is striking because the models indicate that small planets subjected to such intense irradiation for billions of years should have lost their gases long ago. NASA reminds us, however, that some worlds of this type show signs that they are not simple bare rocks. That nuance opened the door to thinking that the low density could be due, in part, to a volume inflated by a substantial layer of gases. To test the idea of ​​a dense atmosphere, the team turned to a technique that James Webb has used on other rocky worlds: measuring the disappearance of some of the infrared glow as the planet passes behind its star. Using the NIRSpec spectrograph, the researchers estimated the temperature of the illuminated hemisphere and compared it to what would be expected for a surface without heat-distributing gases. If TOI-561 b were a bare rock, its temperature would be around 2,700 ºC. However, observations placed that value close to 1,800°C, a difference too large to ignore. The unexpectedly low temperature makes sense if TOI-561 b is enveloped by a dense, volatile-filled atmosphere. In that case, the winds would transport heat from the illuminated hemisphere to less hot areas, which would reduce the infrared emission received by the telescope. Gases capable of absorbing part of the radiation before it escapes into space also come into play, something that coincides with the models evaluated by the team. YoIt is even possible that silicate clouds exist that reflect the light of the star and contribute to cooling the upper layers of the atmosphere. To explain how TOI-561 b maintains such a resilient atmosphere, the researchers propose a mechanism in which magma and gases are in constant exchange. Tim Lichtenberg points out that as the interior releases volatile compounds into the atmosphere, the ocean of molten rock recaptures some of them, reducing the loss to space. This process requires a planet exceptionally rich in volatile substances, very different from Earth in its initial composition. In Lichtenberg’s words, it would be “like a ball of wet lava,” a description that well sums up the extreme nature of the find. The observations that have allowed us to reconstruct this scenario are part of James Webb’s General Observers 3860 program. For more than 37 hours, the telescope continuously tracked the system as TOI-561 b completed nearly four full orbits, a record that offers a rare glimpse of how its brightness varies along the way. With that volume of data, the team is now analyzing how the temperature changes around the planet and what clues it provides about the composition of its atmosphere. This set of data, still being analyzed, points to a more complex world than was intuited in the first observations. The case of TOI-561 b shows that even the most extreme worlds can hold surprises. Far from just a scorched rock, Webb’s observations describe a dynamic system in which magma, atmosphere, and stellar radiation interact in ways we don’t yet fully understand. As Johanna Teske points out, “What’s really exciting is that this new data set It’s opening even more questions than it’s answering.“The research continues, and each new analysis seems to confirm that this planet belongs to a category that we are only beginning to know. Artistic images | POT In Xataka | We already know when the interstellar comet 3I/ATLAS will be closest to Earth and what’s … Read more

The James Webb captures a lonely object of the size of Jupiter devouring like a miniature sun

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An international astronomer team has witnessed an extraordinary event: a lonely object, with a mass of just 5 to 10 times that of Jupiter, has entered a violent and prolonged growth burst. Using the combined power of James Webb Space Telescope (JWST) and him Vary Large Telescope (VLT) of the Southern European Observatory, scientists They have observed How this object, known as Cha J11070768-7626326, drastically increases its brightness and its “food” rhythm, behaving like a miniature star. The importance. This discovery represents the first time that a outbreak of accretion of type “exor”, a phenomenon so far associated with young stars, in a body of planetary mass. The finding is not only a milestone in astronomical observation, but also further blur the borders between what we consider a giant planet and a small star. The mystery. CH 1107-7626 is not a planet in the traditional sense that we all have in our mind. Although it has a mass comparable to that of a gaseous giant, I do not orbit any star and is 620 light years from the earth. Is what is known as an “free planetary mass object” or FFPMO (for its acronym in English). The existence of these lonely bodies raises a fundamental question for astronomy: are giant planets that were expelled from their solar systems, or are smaller stars that can exist in isolation? In order to solve this enigma that astronomers have right now on the table, you have to analyze the gas and dust disc that is around, as well as the way of accumulating the material. The fact that Cha 1107-7626 has an album and feeds on it suggests that its origin is more like that of a star. A cosmic feast. Astronomers observed Cha 1107-7626 in a state of calm in April and May 2025. However, for June, something had changed drastically. The object entered a “indulgence.” This means that its rhythm of ‘food’ began to increase, and in this way it reached a mass increase rate of 10-7 masses of Jupiter per year, the highest ever measured in a planetary mass object. As a result of this frenzy, the objective became between 1.5 and 2 brighter magnitudes in visible light and its optical flow increased between 3 and 6 times. This outbreak remained active for at least two months, since it was still on the end of the observation campaign in August 2026. But the most interesting thing is the speed it has. According to the observations made with the Vray Lark Telescope of the European Observatory, the growth rate is really aggressive, with a record rate of devouring 6,600 million tons per second of dust and gas. Great footprints. Beyond the increase in brightness, the telescopes captured detailed physical changes that reveal the nature of the event. A hydrogen emission line, known as Hα, developed a “double peak” profile with a red displaced absorption. According to the authors, this profile is a “distinctive brand” of the accretion channeled through magnetic fields, a process called “magnetospherical accretion” observed in young stars. But the most surprising finding was the change in the chemistry of the disc. At first, changes in the emission lines of the hydrocarbons molecules that came from the disc during the outbreak were seen. But water vapor also began to appear with a characteristic emission around 6.6 µm. This appeared during the outbreak where there was nothing before and is relevant because it is the first time that chemical changes of this type are observed caused by an increase in accretion. Relevance. This event classifies Cha 1107-7626 as the first “exor” of known planetary mass. Exor outbursts are significant accretion events that are considered key episodes in the early evolution of the stars. They can deeply affect the physical structure and chemical composition of the protoplanetary disk, potentially influencing the early stages of planet formation. Observing this process in such a small object demonstrates that the violent and fundamental mechanisms that the stars build also work at planetary scales. The study of Cha 1107-7626 offers an unprecedented vision of the accretion in the lower mass objects of the universe, providing a new window to understand how both smaller stars and the largest planets are formed. Images | Javier Miranda In Xataka | The most transformer of modern cosmology is just around the corner, according to the hypothesis of these physicists

With the James Webb we have seen the oldest black hole in the universe. But you just have more questions

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He James Webb Space Telescope has accustomed us to discoveries that break with our schemes mental The last discovery Where he has been the protagonist, he has undoubtedly re -rethink what we knew about the universe, by confirming the existence of the black hole more distant ever observed. Something that will allow answering some questions that astronomy still had. A colossus that has already been baptized. This black hole has received the name of Capers-lrd-Z9 And it is 13,300 million light years away, which means that we are seeing it as it was just 500 million years after big Bang. In this way, its existence, and especially the size it has, challenges everything we thought about how these giants grow. How this black hole was found. Finding something that is so far is not a simple task precisely. Astronomers used program data Capers (Candels-Aea Prism Epoch of Reion Survey) of the James Webb space telescope, specially designed for explore the confines of the universe. The leader of the research team, Anthony Taylor, Explain that “when looking for black holes, this is the farthest that can be reached in practice. We are really expanding the limits of what current technology can detect.” A discovery to confirm. The key to confirmation was spectroscopy, the technique that breaks down the light of an objective in its different wavelengths, such as a prism. For Identify an active black holescientists are looking for an unmistakable firm: gas that moves at extreme speeds. Turning the spiral towards the black hole, the light of the gas that moves away from us will tend towards a red wavelength, and that of the gas approaching is compressed towards the blue length. In this way, if these two trends are found, it is quite unmistakable that a black hole is ‘seeing’. In this way, the Nirspec Spectrograph The Webb detected a remarkably wide hydrogen emission line, the irrefutable test that a massive object was stirring the gas around it at speeds of up to 3,500 km/s. It belonged to something bigger. Initially, Capers-LRD-Z9 was just an intriguing motorcycle in webb images. However, it was belonging to a new and enigmatic class of objects called ‘Small red points’ (Little Red Dots or LRDS). These galaxiespresent only in the first 1.5 billion years of the universe, they are extremely compact, bright and as its name indicates very red. His discovery was “a big surprise,” according to Steven Finkelstein, co -author of the study. “They didn’t look anything like galaxies seen with Hubble.” In this way, this finding has helped explain two of the great mysteries above the table. Why are they so bright? Its brightness would suggest an unlikely number of stars for such an early era of the universe. In this way, this study confirms the theory that light comes from a supermassive black hole that is active and literally devours the subject. Something that results in hot and shines with a huge intensity. Why are they so red? The model that best suits the observations of Capers-LRD-Z9 suggests that the black hole is wrapped in a dense and neutral gas environment. This gas cloud absorbs the blue light and lets the red pass, staining the entire galaxy. Something that could be confirmed when comparing this object with other similar sources of energy. An impossible giant. The most shocking of Capers-LRD-Z9 is the size of its black hole. It is estimated that it could have a mass of up to 300 million times that of our sun. To put it in perspective, it is so massive that it could represent more than 4.5% of the total mass of all the stars of its host galaxy, a proportion much greater than the 0.1% we see in the nearby galaxies. How could it grow so much and so fast? This is one of the big questions that anyone can ask, taking into account that this black hole appeared at a very early stage of the universe. Something that questions the current models that we have on the table. Finkelstein summarizes it as follows: “This adds to the growing evidence that primitive black holes grew much faster than we thought were possible. Or they began being much more massive than our models predict.” Two models to explain its existence. The first of these is that the black hole was not born from a star, but from the direct collapse of a cloud of primary gas, starting its life with a mass of thousands of soles and growing at a normal pace. The second theory that scientists have on the table is that it was actually born from one of the first massive stars (with a mass 100 times higher than the sun) that existed. The question here is that he would have grown at a rhythm ‘Super-Edington‘, devouring matter much faster than the stable theoretical limit is considered. There is still much to find out. The team expects to obtain more observations with the Webb to unravel the secrets of this single object. “We had not been able to study the early evolution of black holes until recently,” concludes Taylor, “and we are excited to see what we can learn.” Images | Nasa Hubble Space Telescope In Xataka | Two astronomers studied the “sound of the Big Bang” and reached a disturbing conclusion: the earth is in a lonely bubble

The James Webb has just photographed one of the great mysteries of the universe’s galaxies: how they intertwine

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How many galaxies fit in an image? In the instruments of the James Webb space telescope (JWST), at least, many: hundreds. And even thousands. From close to the distant. The image taken by the JWST (with the help of the veteran hubble) and published by the European Space Agency (ESA) It shows us objects in a wide range of distances: from stars located within our own galaxy (easy to distinguish thanks to The characteristics six points of diffraction of this telescope) to distant galaxies in space and in time. The “star” of the image. However, according to Explain the agency itselfthe main protagonist of this capture is none other than a cluster of galaxies that we can see below the center of the image, a distant group of galaxies that shines in a mixture tone of white and gold. This group emerged about 6.5 billion years after the Big Bang, when the universe as and as we know it was somewhat less than the age it is now. The importance of this group lies in the fact that more than half of the galaxies we know can be found in similar groups, so studying it can help us understand more about how these groups that make up the greatest structures linked through the force of gravity are formed, says ESA. Cosmos-Web. The outstanding group is the largest galactic cluster in the region called Cosmos-Web Field. COSMOS (Cosmic Evolution Survey) It is a survey that uses telescopes such as webb, hubble or the XMM-Newton Space Observatory of ESA to explore the spaces and space phenomena that occurred in that celestial region. He Cosmos-Web program It seeks to take advantage of the high abilities of the JWST and instruments such as the Nircam filters on board to explore and map an area of ​​0.54 square degrees of the celestial vault, a little more than twice and a half times the area that occupies the full moon in our sky. This power of the instruments of the orbital telescope should allow us to understand how galactic clusters formed, taking us at a time when the universe was only 1.9 billion years old, 14% of their current age. This is intended to meet three objectives: identify galaxies at the time of reion (when the first stars were “caught”; probe the formation of the most massive galaxies; and understand the relationship between the mass of the stars in a galaxy and The galactic halo that “wraps.” “Galaxies feast ”. In its publication, ESA has given some additional details about the image we see. They explain, this combines nircam images (Near-Infrared Camera) with Hubble observations to present ourselves “a visual feast of galaxies.” In capture They can be seen galaxies of different types and even pairs of galaxies in the process of merging. The European Agency He also explains The interpretation of the colors of the galaxies: the galaxies that tend to the bluish tones are those in which young stars predominate, while the most old are older; either because of the color of the stars inside, either because they are further in space and therefore in time. The latter is the effect of the phenomenon called Redshift or red shift. Galactic evolution. Images like this have to tell us about the evolution of the universe and, above all, of galaxies like ours. The gravitational interaction between galaxies (more or less) close affects what happens within the same galaxies, such is the mass that these groups accumulate. And not only that: collisions and mergers between galaxies in the same group also condition what happens in these. An example can find it when the nearby step of two galaxies of different size allows a huge clouds of matter “start”, or it can Cause a “burst” that quickly consumes the gas of this. In Xataka | The James Webb has found a galaxy when the universe was 330 million years old. Hide an entire enigma Image | Es es/Webb, Nasa & Csa, G. Gozaliasl, A. Koekemoer, M. Franco, and The Cosmos-Web Team

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