A windows 8-like Task Manager for Windows 7 ,work in progress!
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By Big John Studd · Posted
The sweet release of death has never looked more appealing. -
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By MrElectrifyer · Posted
Meh, just another dongle-haven downgrade compared to my Surface Pro 7+. Whenever I decide to upgrade in the next decade or so, it certainly won't be another microslop Surface with this enshitification trend they've been having after the Surface Pro 7+. Hopefully a future generation of the Framework 12 will be a real upgrade... -
By hellowalkman · Posted
This could exactly be how our Sun ends but it's not as simple by Sayan Sen Image by Drew Rae via Pexels An international team led by Université de Montréal (University of Montreal) PhD student Érika Le Bourdais has found that the ancient white dwarf star LSPM J0207+3331 is still pulling in planetary debris, even though it has been cooling for about three billion years. White dwarfs are dense, Earth-sized stellar remnants left behind when Sun-like stars exhaust their nuclear fuel and shed their outer layers. The star, located 145 light-years away in the constellation Triangulum, is the oldest and coldest white dwarf known to have a surrounding disk of dust. The star was first spotted in 2019 by a citizen scientist through the Backyard Worlds: Planet 9 project. Its cool temperature immediately suggested that it was very old, since white dwarfs gradually lose heat over time. Using the W. M. Keck telescopes in Hawaii, astronomers later confirmed that the star shows infrared signals consistent with dust rings formed by asteroids breaking apart under its strong gravity. Such infrared excesses occur when a star emits more infrared light than expected, often because warm dust surrounding it absorbs and re-radiates energy. “This discovery challenges our understanding of planetary system evolution,” said Le Bourdais. “The fact that we still see planetary debris being accreted three billion years after the star became a white dwarf suggests that asteroids, comets, and even planets can remain in orbit around these stars for a very long time.” Spectroscopic analysis—a technique that studies light to identify the chemical elements present in an object—revealed thirteen heavy elements in the star’s atmosphere: sodium, magnesium, aluminium, silicon, calcium, titanium, chromium, manganese, iron, cobalt, nickel, copper, and strontium. Normally, heavy elements sink quickly in hydrogen-rich white dwarfs, making them hard to detect. “We expected to see only a few elements, but we found dozens!” explained Le Bourdais. The research paper adds more detail. The absence of carbon features suggests the debris came from a carbon-volatile-depleted source. The abundance pattern shows slight deficits of magnesium and silicon compared to iron but otherwise resembles Earth-like material. This points to a differentiated rocky body—one whose materials have separated into distinct layers such as a metallic core and rocky mantle—with a metallic core fraction higher than Earth’s. In other words, the star is accreting the remains of a large rocky object, similar in structure to Earth or the asteroid Vesta. “White dwarfs offer one of the only ways we can directly measure the composition of exoplanets,” said Patrick Dufour, co-author and professor at Université de Montréal. “When planetary debris come too close, they are torn apart by the star’s gravity and end up polluting its atmosphere, leaving a detailed chemical fingerprint of its composition.” The team also detected weak Ca II H & K line core emission, making this only the second known isolated polluted white dwarf to show this feature. These are specific spectral signatures produced by ionised calcium and can indicate unusual physical activity in a star’s upper atmosphere. The finding suggests that extra physical processes may be happening in or above the star’s upper atmosphere. The study stresses the importance of including heavy elements in model atmosphere calculations, since leaving them out can distort the inferred structure and lead to inaccurate stellar parameters. Earlier work suggested the star’s infrared excess came from two dust rings. The new analysis shows that a single silicate dust disk—a ring composed largely of rock-forming minerals rich in silicon and oxygen—can explain the observed signal at 11.6 μm, simplifying the picture of the system’s structure. The question of how debris ended up falling into the star so late remains open. One idea is that giant planets in the system slowly destabilised smaller bodies over billions of years. Another possibility is that a passing star disturbed the orbits of debris. “Future observations with the James Webb Space Telescope or archival data found in the European Space Agency’s Gaia mission could help distinguish between a planetary rearrangement and the gravitational effect of a close stellar encounter,” said John Debes, co-author and researcher at the Space Telescope Science Institute. Dufour noted that hydrogen-rich white dwarfs are the most common type, and the coolest among them are the oldest stars in the galaxy. “We didn't have the habit of looking for signs of accretion in them. This unique case motivates us to expand our search to more of these stars.” The findings show that even after billions of years, planetary systems can remain active and complex. Substantial accretion events—the gradual accumulation of surrounding material onto a celestial object—can still occur long after a star’s death, offering a rare window into the composition and fate of distant worlds. Source: University of Montreal, IOPScience This article was generated with some help from AI and reviewed by an editor. Under Section 107 of the Copyright Act 1976, this material is used for the purpose of news reporting. Fair use is a use permitted by copyright statute that might otherwise be infringing. -
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