Soup Posted at 2024-11-11 23:49:59(6Wks ago) Report Permalink URL | ||
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| Mining old data from NASA's Voyager 2 solves several Uranus mysteries by Karen Fox, Molly Wasser and Gretchen McCartney, NASA  The first panel of this artist’s concept depicts how Uranus’s magnetosphere — its protective bubble — was behaving before the flyby of NASA’s Voyager 2. The second panel shows an unusual kind of solar weather was happening during the 1986 flyby, giving scientists a skewed view of the magnetosphere. Credit: NASA/JPL-Caltech When NASA's Voyager 2 spacecraft flew by Uranus in 1986, it provided scientists' first—and, so far, only—close glimpse of this strange, sideways-rotating outer planet. Alongside the discovery of new moons and rings, baffling new mysteries confronted scientists. The energized particles around the planet defied their understanding of how magnetic fields work to trap particle radiation, and Uranus earned a reputation as an outlier in our solar system. Now, new research analyzing the data collected during that flyby 38 years ago has found that the source of that particular mystery is a cosmic coincidence. It turns out that in the days just before Voyager 2's flyby, the planet had been affected by an unusual kind of space weather that squashed the planet's magnetic field, dramatically compressing Uranus's magnetosphere. "If Voyager 2 had arrived just a few days earlier, it would have observed a completely different magnetosphere at Uranus," said Jamie Jasinski of NASA's Jet Propulsion Laboratory in Southern California and lead author of the new work published in Nature Astronomy. "The spacecraft saw Uranus in conditions that only occur about 4% of the time." Magnetospheres serve as protective bubbles around planets (including Earth) with magnetic cores and magnetic fields, shielding them from jets of ionized gas—or plasma—that stream out from the sun in the solar wind. Learning more about how magnetospheres work is important for understanding our own planet, as well as those in seldom-visited corners of our solar system and beyond. That's why scientists were eager to study Uranus's magnetosphere, and what they saw in the Voyager 2 data in 1986 flummoxed them. Inside the planet's magnetosphere were electron radiation belts with an intensity second only to Jupiter's notoriously brutal radiation belts. But there was apparently no source of energized particles to feed those active belts; in fact, the rest of Uranus's magnetosphere was almost devoid of plasma. The missing plasma also puzzled scientists because they knew that the five major Uranian moons in the magnetic bubble should have produced water ions, as icy moons around other outer planets do. They concluded that the moons must be inert with no ongoing activity  NASA’s Voyager 2 captured this image of Uranus while flying by the ice giant in 1986. New research using data from the mission shows a solar wind event took place during the flyby, leading to a mystery about the planet’s magnetosphere that now may be solved. Credit: NASA/JPL-Caltech Solving the mystery So why was no plasma observed, and what was happening to beef up the radiation belts? The new data analysis points to the solar wind. When plasma from the sun pounded and compressed the magnetosphere, it likely drove plasma out of the system. The solar wind event also would have briefly intensified the dynamics of the magnetosphere, which would have fed the belts by injecting electrons into them. The findings could be good news for those five major moons of Uranus: Some of them might be geologically active after all. With an explanation for the temporarily missing plasma, researchers say it's plausible that the moons actually may have been spewing ions into the surrounding bubble all along. Planetary scientists are focusing on bolstering their knowledge about the mysterious Uranus system, which the National Academies' 2023 Planetary Science and Astrobiology Decadal Survey prioritized as a target for a future NASA mission. JPL's Linda Spilker was among the Voyager 2 mission scientists glued to the images and other data that flowed in during the Uranus flyby in 1986. She remembers the anticipation and excitement of the event, which changed how scientists thought about the Uranian system. "The flyby was packed with surprises, and we were searching for an explanation of its unusual behavior. The magnetosphere Voyager 2 measured was only a snapshot in time," said Spilker, who has returned to the iconic mission to lead its science team as project scientist. "This new work explains some of the apparent contradictions, and it will change our view of Uranus once again." Voyager 2, now in interstellar space, is almost 13 billion miles (21 billion kilometers) from Earth. | |
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| SoupPosted at 2024-11-18 20:57:50(5Wks ago) Report Permalink URL | ||
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| Theoretical astrophysicist proposes solution to enigma of Crab Nebula's 'zebra' pattern by Brendan M. Lynch, University of Kansas  Crab Nebula. Credit: NASA A theoretical astrophysicist from the University of Kansas may have solved a nearly two-decade-old mystery over the origins of an unusual "zebra" pattern seen in high-frequency radio pulses from the Crab Nebula. His findings have just been published in Physical Review Letters. The Crab Nebula features a neutron star at its center that has formed into a 12-mile-wide pulsar pinwheeling electromagnetic radiation across the cosmos. "The emission, which resembles a lighthouse beam, repeatedly sweeps past Earth as the star rotates," said lead author Mikhail Medvedev, professor of physics & astronomy at KU. "We observe this as a pulsed emission, usually with one or two pulses per rotation. The specific pulsar I'm discussing is known as the Crab Pulsar, located in the center of the Crab Nebula 6,000 light years away from us." The Crab Nebula is the remnant of a supernova that appeared in 1054. "Historical records, including Chinese accounts, describe an unusually bright star appearing in the sky," said the KU researcher. But unlike any other known pulsar, Medvedev said the Crab Pulsar features a zebra pattern—unusual band spacing in the electromagnetic spectrum proportional to band frequencies, and other weird features like high polarization and stability. "It's very bright, across practically all wave bands," he said. "This is the only object we know of that produces the zebra pattern, and it only appears in a single emission component from the Crab Pulsar. "The main pulse is a broadband pulse, typical of most pulsars, with other broadband components common to neutron stars. However, the high-frequency interpulse is unique, ranging between 5 and 30 gigahertz—frequencies similar to those in a microwave oven." Since this pattern was discovered in a 2007 paper, the KU researcher said the pattern had proved "baffling" for investigators.  Medvedev modeled wave diffraction off a circular reflecting region with radially varying index of refraction outside of it to better understand the Crab Nebula's zebra pattern. Credit: Mikhail Medvedev "Researchers proposed various emission mechanisms, but none have convincingly explained the observed patterns," he said. Using data from the Crab Pulsar, Medvedev established a method using wave optics to gauge the density of the pulsar's plasma—the "gas" of charged particles (electrons and positrons)—using a fringe pattern found in the electromagnetic pulses. "If you have a screen and an electromagnetic wave passes by, the wave doesn't propagate straight through," Medvedev said. "In geometrical optics, shadows cast by obstacles would extend indefinitely—if you're in the shadow, there's no light; outside of it, you see light. But wave optics introduces a different behavior—waves bend around obstacles and interfere with each other, creating a sequence of bright and dim fringes due to constructive and destructive interference." This well-known fringe pattern phenomenon is caused by consistent constructive interference but has different characteristics when radio waves propagate around a neutron star. "A typical diffraction pattern would produce evenly spaced fringes if we just had a neutron star as a shield," the KU researcher said. "But here, the neutron star's magnetic field generates charged particles constituting a dense plasma, which varies with distance from the star. | |
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| SoupPosted at 2024-11-19 00:46:17(5Wks ago) Report Permalink URL | ||
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| Hubble sees aftermath of galaxy's scrape with Milky Way by NASA  This artist's concept shows the Large Magellanic Cloud, or LMC, in the foreground as it passes through the gaseous halo of the much more massive Milky Way galaxy. The encounter has blown away most of the spherical halo of gas that surrounds the LMC, as illustrated by the trailing gas stream reminiscent of a comet's tail. Still, a compact halo remains, and scientists do not expect this residual halo to be lost. The team surveyed the halo by using the background light of 28 quasars, an exceptionally bright type of active galactic nucleus that shines across the universe like a lighthouse beacon. Their light allows scientists to "see" the intervening halo gas indirectly through the absorption of the background light. The lines represent the Hubble Space Telescope's view from its orbit around Earth to the distant quasars through the LMC's gas. Credit: NASA, ESA, Ralf Crawford (STScI) A story of survival is unfolding at the outer reaches of our galaxy, and NASA's Hubble Space Telescope is witnessing the saga. The Large Magellanic Cloud, also called the LMC, is one of the Milky Way galaxy's nearest neighbors. This dwarf galaxy looms large on the southern nighttime sky at 20 times the apparent diameter of the full moon. Many researchers theorize that the LMC is not in orbit around our galaxy, but is just passing by. These scientists think that the LMC has just completed its closest approach to the much more massive Milky Way. This passage has blown away most of the spherical halo of gas that surrounds the LMC. Now, for the first time, astronomers have been able to measure the size of the LMC's halo—something they could do only with Hubble. In a new study, available on the preprint server arXiv and to be published in The Astrophysical Journal Letters, researchers were surprised to find that it is so extremely small, about 50,000 light-years across. That's around 10 times smaller than halos of other galaxies that are the LMC's mass. Its compactness tells the story of its encounter with the Milky Way. "The LMC is a survivor," said Andrew Fox of AURA/STScI for the European Space Agency in Baltimore, who was principal investigator on the observations. "Even though it's lost a lot of its gas, it's got enough left to keep forming new stars. So new star-forming regions can still be created. A smaller galaxy wouldn't have lasted—there would be no gas left, just a collection of aging red stars." Though quite a bit worse for wear, the LMC still retains a compact, stubby halo of gas—something that it wouldn't have been able to hold onto gravitationally had it been less massive. The LMC is 10 percent the mass of the Milky Way, making it heftier than most dwarf galaxies. "Because of the Milky Way's own giant halo, the LMC's gas is getting truncated, or quenched," explained STScI's Sapna Mishra, the lead author on the paper chronicling this discovery. "But even with this catastrophic interaction with the Milky Way, the LMC is able to retain 10 percent of its halo because of its high mass." A gigantic hair dryer Most of the LMC's halo was blown away due to a phenomenon called ram-pressure stripping. The dense environment of the Milky Way pushes back against the incoming LMC and creates a wake of gas trailing the dwarf galaxy—like the tail of a comet. "I like to think of the Milky Way as this giant hairdryer, and it's blowing gas off the LMC as it comes into us," said Fox. "The Milky Way is pushing back so forcefully that the ram pressure has stripped off most of the original mass of the LMC's halo. There's only a little bit left, and it's this small, compact leftover that we're seeing now."  This artist's concept illustrates the Large Magellanic Cloud's (LMC's) encounter with the Milky Way galaxy's gaseous halo. In the top panel, at the middle of the right side, the LMC begins crashing through our galaxy's much more massive halo. The bright purple bow shock represents the leading edge of the LMC's halo, which is being compressed as the Milky Way's halo pushes back against the incoming LMC. In the middle panel, part of the halo is being stripped and blown back into a streaming tail of gas that eventually will rain into the Milky Way. The bottom panel shows the progression of this interaction, as the LMC's comet-like tail becomes more defined. A compact LMC halo remains. Because the LMC is just past its closest approach to the Milky Way and is moving outward into deep space again, scientists do not expect the residual halo will be lost. Credit: NASA, ESA, Ralf Crawford (STScI) As the ram pressure pushes away much of the LMC's halo, the gas slows down and eventually will rain into the Milky Way. But because the LMC has just gotten past its closest approach to the Milky Way and is moving outward into deep space again, scientists do not expect the whole halo will be lost. Only with Hubble To conduct this study, the research team analyzed ultraviolet observations from the Mikulski Archive for Space Telescopes at STScI. Most ultraviolet light is blocked by the Earth's atmosphere, so it cannot be observed with ground-based telescopes. Hubble is the only current space telescope tuned to detect these wavelengths of light, so this study was only possible with Hubble. The team surveyed the halo by using the background light of 28 bright quasars. The brightest type of active galactic nucleus, quasars are believed to be powered by supermassive black holes. Shining like lighthouse beacons, they allow scientists to "see" the intervening halo gas indirectly through the absorption of the background light. Quasars reside throughout the universe at extreme distances from our galaxy. The scientists used data from Hubble's Cosmic Origins Spectrograph (COS) to detect the presence of the halo's gas by the way it absorbs certain colors of light from background quasars. A spectrograph breaks light into its component wavelengths to reveal clues to the object's state, temperature, speed, quantity, distance, and composition. With COS, they measured the velocity of the gas around the LMC, which allowed them to determine the size of the halo. Because of its mass and proximity to the Milky Way, the LMC is a unique astrophysics laboratory. Seeing the LMC's interplay with our galaxy helps scientists understand what happened in the early universe, when galaxies were closer together. It also shows just how messy and complicated the process of galaxy interaction is. Looking to the future The team will next study the front side of the LMC's halo, an area that has not yet been explored. "In this new program, we are going to probe five sightlines in the region where the LMC's halo and the Milky Way's halo are colliding," said co-author Scott Lucchini of the Center for Astrophysics | Harvard & Smithsonian. "This is the location where the halos are compressed, like two balloons pushing against each other." | |
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| SoupPosted at 2024-11-28 00:14:43(3Wks ago) Report Permalink URL | ||
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| Investigating how the biggest galaxies in the cosmos grew so quickly before dying by Jonathan O'Callaghan, Horizon: The EU Research & Innovation Magazine  The formation of galaxies in the universe should follow a fairly simple path. It starts with small galaxies, which then grow bigger and bigger until they become the giant galaxies we see in the modern universe, like our Milky Way. Easy, right? But that is not strictly true for a particular class of elliptical galaxies—huge spherical collections of stars without a clear structure. With the help of EU funding, researchers have set out to discover the origin of these galaxies and unlock more mysteries of the universe. To do that, they have traveled back in time, using powerful telescopes that can follow light to remote corners of the universe. This has allowed scientists to look at galaxies as they appeared in the past, even billions of years ago. "Galaxies are the flag posts of the universe. They are the origins of everything," said Sune Toft, a cosmologist at the Niels Bohr Institute in Denmark. "Understanding the detailed formation scenarios is the only way to understand the beginning of the universe and where we come from." Toft led the EU-funded ConTExt project from 2015 to 2021. The goal was to observe some of the oldest elliptical galaxies possible, stretching back into the first 2 billion years of the 13.8-billion-year history of the universe. Time travel to remote dark corners: no answers yet Although researchers have gained some insight into elliptical galaxies, they remain a mystery. "These have been known for many years, but it's kind of a conundrum how they form because they are uniformly old and dead in the local universe," Toft said. The thinking behind his research was this: as we look further back in time, by observing galaxies that are billions of light years away, at some point we should start to see the progenitors of these galaxies and be able to explain how they were able to grow so massive. "But the further away we looked, they kept looking old and dead. They have virtually no star formation," said Toft, referring to the process at the core of galaxies' evolution. That meant the galaxies must have grown very quickly in the early universe. Still, it remains unknown exactly how and when. And there is another riddle: if the galaxies grew quickly, why did they stop growing? And what did that mean for our understanding of hierarchical galaxy structure in the universe, which comprises stars, planetary systems, star clusters and galaxies? "The small galaxies are supposed to form first. So why are these massive galaxies the first ones to form?" Toft said. Star formation His hypothesis was that these galaxies might have undergone intense star formation early on in their history, becoming what are known as starburst galaxies. Starburst galaxies have extremely dense amounts of dust and gas and can form stars thousands of times the mass of our sun every year. Our Milky Way, by comparison, forms one new solar mass per year on average. Using a telescope in Chile called the Atacama Large Millimeter Array, as well as the Hubble Space Telescope and Spitzer Space Telescope, both of which orbited the Earth at the time, Toft set to work. He found that, in the first 1 to 2 billion years after the Big Bang, "there were enough of these star-forming galaxies to turn into the dead galaxies." These galaxies were dense and compact and looked similar to the cores of elliptical galaxies we see today. Toft worked on the premise that these progenitor elliptical galaxies formed quickly in the universe before something shut off their star formation. Then, over the next 10 billion or so years, they gradually accumulated more stars by gobbling up smaller galaxies, adding their stars to the galaxy's outer regions. Thus, the elliptical galaxies remained old and dead, but could still grow to immense sizes. The early growth of the ellipticals was likely caused by galaxy mergers that ignited star formation. "You have two major galaxies going head-on into each other, and the gas gets compressed into the center of this collision," said Toft. "This is what you need to have very high star formation rates." But what was still not clear was how these galaxies switched off. How did they stop forming stars so quickly and eventually become the dead galaxies we see today? Quenching Sirio Belli, an astronomer at the University of Bologna in Italy, is investigating this problem with his Red Cardinal project, an EU-funded initiative running from 2023 to 2028. It is using the powerful James Webb Space Telescope (JWST), which orbits the sun, to probe these early galaxies like never before. The emerging idea is that black holes found at the centers of these galaxies are responsible for their evolution. Almost all galaxies today, including our own, contain a supermassive black hole at their center, a huge object millions to billions of times the mass of our sun. These black holes drive the formation and evolution of a galaxy, churning and expelling gas and dust throughout a galaxy's history. Belli has found that these black holes might also be responsible for stopping star formation in early galaxies, in a process referred to as quenching. In April 2024, his team used JWST to report the discovery of a massive galaxy undergoing quenching about 2.6 billion years after the Big Bang. "It's a lucky coincidence because we observed this galaxy exactly when quenching was happening," he said. The galaxy appeared to have been growing until recently. "It just stopped forming stars," said Belli. "At the same time, we found this giant wind coming out of the galaxy. We think this is due to the supermassive black hole at the center of the galaxy." The idea is that the black hole became extremely active, which "pushed the gas away from the galaxy," said Belli. "So you don't have any gas to form new stars. It's like a car that runs out of fuel." What is unclear is exactly why the black hole became active. One possibility is that once the black hole eats enough material and gains enough mass, it suddenly starts releasing a lot of energy, causing quenching. "We think that once a galaxy reaches a certain mass, 100 billion solar masses, they are then eventually all quenched," said Belli. "We don't see any massive galaxy in today's universe that is still forming stars." An extremely large telescope to probe further More answers might come from new telescopes like the European Extremely Large Telescope (ELT), which is being built in Chile and due to begin its observations in 2028. "With the ELT, we can look in detail inside these galaxies" in the early universe, said Belli, something JWST is not able to do. That will tell researchers the overall star formation rate, but also "where the stars are being formed," he said. "If the ELT works as promised, it should be pretty cool." Determining the mechanism of the quenching process will be crucial in unraveling the enigma of why galaxies die, an issue that continues to perplex scientists. "It shouldn't be possible because when a galaxy is in the early universe, it's filled with gas," said Toft. "How do you go from forming thousands of solar masses per year to nothing? If we want to prove black holes are responsible, we have to find galaxies right in the process of shutting down." With that understanding, we will learn how the cosmos as we see it today came to be. | |
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| SoupPosted at 2024-12-03 00:07:16(3Wks ago) Report Permalink URL | ||
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| Interstellar objects can't hide from Vera Rubin by Brian Koberlein, Universe Today  Artist impression of the interstellar comet 2I/Borisov as it travels through our solar system. Credit: NRAO/AUI/NSF, S. Dagnello We have studied the skies for centuries, but we have only found two objects known to come from another star system. The first interstellar object to be confirmed was 1I/2017 U1, more commonly known as 'Oumuamua. It was discovered with the Panoramic Survey Telescope and Rapid Response System (Pan-STARRS) and stood out because of its large proper motion. Because 'Oumuamua swept through the inner solar system, it was relatively easy to distinguish. The second interstellar object, 2I/Borisov, stood out because it entered the inner solar system from well above the orbital plane. But while we have only discovered two alien visitors so far, astronomers think interstellar objects are common. It's estimated that several of them visit our solar system each year, and there may be thousands within the orbit of Neptune on any given day. They just don't stand out, so we don't notice them. But that could soon change. The Vera C. Rubin Observatory is scheduled to come online in 2025. Unlike many large telescopes, Rubin Observatory isn't designed to focus on specific targets in the sky. Its mirror can capture a patch of sky seven moons wide in a single image. It will capture more than a petabyte of data every night, capturing images of solar system bodies every few days. This will allow astronomers to track even faint and slow-moving bodies with precision. The orbit of any interstellar object will stand out clearly. If astronomers can find them. Which is where a new study published in Astronomy & Astrophysics comes in. With so much data being gathered, there is no way to go through the data by hand. Some things, such as supernovae and variable stars, will be easy to distinguish, but interstellar bodies in the outer solar system will pose a particular challenge. In any given image, they will appear as a common asteroid or comet. It's only after months or years of tracking that their unique orbits will reveal their true origins. So the authors of this new work propose using machine learning. To demonstrate how this would work, the team created a database of simulated solar system bodies. Some of them were given regular orbits, while others were given interstellar paths. Based on this data, they trained algorithms to distinguish the two. They found that some machine learning methods worked better than others. In this case, the Random Forest approach, where one classifies decision trees statistically, and the Gradient Boosting method, which prioritizes "weak learners" to strengthen them, seem to work the best. The more commonly known Neural Network method was less effective. Overall, the team found that machine learning can detect interstellar objects with great efficiency, and the number of false positives should be small enough that they could be effectively managed. While the approach won't find all the interstellar bodies in our solar system, it should be able to find hundreds of them within the first year of Rubin's operation. And that will give us plenty of data to better understand these enigmatic visitors. | |
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| SoupPosted at 2024-12-03 21:14:48(2Wks ago) Report Permalink URL | ||
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| Webb observations discover new planet in Kepler-51 'super-puff' system by Pennsylvania State University  Illustration of the Kepler-51 system and its inner three planets, which have unusually low density. New observations from NASA's James Webb Space Telescope suggest that at least one more planet is in the system. Credit: NASA, ESA, and L. Hustak, J. Olmsted, D. Player and F. Summers (STScI) An unusual planetary system with three known ultra-low density "super-puff" planets has at least one more planet, according to new research led by researchers from Penn State and Osaka University. The research team set out to study Kepler-51d, the third planet in the system, with NASA's James Webb Space Telescope (JWST) but almost missed their chance when the planet unexpectedly passed in front of its star two hours earlier than models predicted. After scrutinizing new and archival data from a variety of space and Earth-based telescopes, the researchers found that the best explanation is the presence of a fourth planet, whose gravitational pull impacts the orbits of the other planets in the system. The new planet's discovery is detailed in a paper appearing in The Astronomical Journal. "Super puff planets are very unusual in that they have very low mass and low density," said Jessica Libby-Roberts, Center for Exoplanets and Habitable Worlds Postdoctoral Fellow at Penn State and co-first author of the paper. "The three previously known planets that orbit the star Kepler-51 are about the size of Saturn but only a few times the mass of Earth, resulting in a density like cotton candy. We think they have tiny cores and huge atmospheres of hydrogen and helium, but how these strange planets formed and how their atmospheres haven't been blown away by the intense radiation of their young star has remained a mystery. We planned to use JWST to study one of these planets to help answer these questions, but now we have to explain a fourth low-mass planet in the system." When a planet passes in front of—or transits—its star when viewed from Earth, it blocks some of the star's light, causing a slight decrease in the star's brightness. The duration and amount of that decrease gives clues to the planet's size and other characteristics. Planets transit when they complete an orbit around their star, but sometimes they transit a few minutes early or late because the gravity from other planets in the system tugs on them. These minor differences are known as transit timing variations and are built into astronomers' models to allow them to accurately predict when planets will transit. The researchers said they had no reason to believe the three-planet model of the Kepler-51 system was inaccurate, and they successfully used the model to predict the transit time of Kepler-51b in May 2023 and followed-up with the Apache Point Observatory (APO) telescope to observe it on schedule. "We also tried to use the Penn State Davey Lab telescope to observe a transit of Kepler-51d in 2022, but some poorly timed clouds blocked our view right as the transit was predicted to start," Libby-Roberts said. "It's possible we could have learned something was off then, but we had no reason to suspect that Kepler-51d wouldn't transit as expected when we planned to observe it with JWST." The team's three-planet model predicted that Kepler-51d would transit around 2 a.m. EDT in June 2023, and the researchers prepared to observe the event with both JWST and APO. "Thank goodness we started observing a few hours early to set a baseline, because 2 a.m. came, then 3, and we still hadn't observed a change in the star's brightness with APO," Libby-Roberts said. "After frantically re-running our models and scrutinizing the data, we discovered a slight dip in stellar brightness immediately when we started observing with APO, which ended up being the start of the transit—2 hours early, which is well beyond the 15-minute window of uncertainty from our models." When the researchers analyzed the new APO and JWST data, they confirmed that they had captured the transit of Kepler-51d, albeit considerably earlier than expected. "We were really puzzled by the early appearance of Kepler-51d, and no amount of fine-tuning the three-planet model could account for such a large discrepancy," said Kento Masuda, associate professor of earth and space science at Osaka University and co-first author of the paper. "Only adding a fourth planet explained this difference. This marks the first planet discovered by transit timing variations using JWST." To help explain what is happening in the Kepler-51 system, the research team revisited previous transit data from NASA's Kepler space telescope and NASA's Transiting Exoplanet Survey Satellite (TESS). They also made new observations of the inner planets in the system, including with the Hubble Space Telescope and the California Institute of Technology's Palomar Observatory telescope, and obtained archival data from several ground-based telescopes. Because the new planet, Kepler-51e, has not yet been observed transiting—perhaps because it may not pass in the line of sight between its star and Earth—the researchers noted how important it was to obtain as much data as possible to support their new models. "We conducted what is called a 'brute force' search, testing out many different combinations of planet properties to find the four-planet model that explains all of the transit data gathered over the past 14 years," Masuda said. "We found that the signal is best explained if Kepler-51e has a mass similar to the other three planets and follows a fairly circular orbit of about 264 days—something we would expect based on other planetary systems. Other possible solutions we found involve a more massive planet on a wider orbit, though we think these are less likely." Accounting for a fourth planet and adjusting the models also changes the expected masses of the other planets in the system. According to the researchers, this impacts other inferred properties about these planets and informs how they might have formed. Although the inner three planets are slightly more massive than previously thought, they are still classified as super puffs. However, it is unclear if Kepler-51e is also a super puff planet, because the researchers have not observed a transit of Kepler-51e and therefore cannot calculate its radius or density. "Super puff planets are fairly rare, and when they do occur, they tend to be the only ones in a planetary system," Libby-Roberts said. "If trying to explain how three super puffs formed in one system wasn't challenging enough, now we have to explain a fourth planet, whether it's a super puff or not. And we can't rule out additional planets in the system either." Because the researchers believe Kepler-51e has an orbit of 264 days, they said that additional observing time is needed to get a better picture of the impacts of its gravity—or that of additional planets—on the three inner planets in the system. "Kepler-51e has an orbit slightly larger than Venus and is just inside the star's habitable zone, so a lot more could be going on beyond that distance if we take the time to look," Libby-Roberts said. "Continuing to look at transit timing variations might help us discover planets that are further away from their stars and might aid in our search for planets that could potentially support life." The researchers are currently analyzing the rest of the JWST data, which could provide information about the atmosphere of Kepler-51d. Studying the composition and other properties of the three inner planets could also improve understanding of how the unusual ultra-low-density super puff planets formed, the researchers said. In addition to Libby-Roberts and Masuda, who led the Kepler-51d team, the international research team includes John Livingston at the National Astronomical Observatory of Japan, who coordinated most of the ground-based follow-ups; many ground-based observers; the Kepler-51b team; and the Palomar team. | |
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| Jase1Posted at 2024-12-16 15:25:51(1Wk ago) Report Permalink URL | ||
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|  Saturn takes more than 29 years to orbit the Sun, and so OPAL has followed it for approximately one quarter of a Saturnian year (picking up in 2018, after the end of the Cassini mission). Because Saturn is tilted 26.7 degrees, it goes through more profound seasonal changes than Jupiter. Saturnian seasons last approximately seven years. This also means Hubble can view the spectacular ring system from an oblique angle of almost 30 degrees to seeing the rings tilted edge-on. Edge-on, the rings nearly vanish because they are relatively paper-thin. This will happen again in 2025. OPAL has followed changes in colors of Saturn's atmosphere. The varying color was first detected by the Cassini orbiter, but Hubble provides a longer baseline. Hubble revealed slight changes from year-to-year in color, possibly caused by cloud height and winds. The observed changes are subtle because OPAL has covered only a fraction of a Saturnian year. Major changes happen when Saturn progresses into the next season. Saturn's mysteriously dark ring spokes, which slice across the ring plane, are transient features that rotate along with the rings. Their ghostly appearance only persists for two or three rotations around Saturn. During active periods, freshly formed spokes continuously add to the pattern. They were first seen in 1981 by Voyager 2. Cassini also saw the spokes during its 13-year-long mission, which ended in 2017. Hubble shows that the frequency of spoke apparitions is seasonally driven, first appearing in OPAL data in 2021. Long-term monitoring shows that both the number and contrast of the spokes vary with Saturn's seasons. This "Warhol-esque" array of Saturn images depicts real data from multiple filters mapped onto the RGB colors perceptible to the human eye. Each filter combination emphasizes subtle differences in cloud altitude or composition. Infrared spectra from the Cassini mission suggested that Saturn's aerosol particles may have even more complex chemical diversity than on Jupiter. The OPAL program extends Cassini's legacy by measuring how the subtle patterns in the clouds vary over time. Image credit: NASA, ESA, Amy Simon (NASA-GSFC), Michael H. Wong (UC Berkeley); Image Processing: Joseph DePasquale (STScI) | |
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| SoupPosted at 2024-12-18 00:55:56(6Days ago) Report Permalink URL | ||
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| First-ever binary star found near our galaxy's supermassive black hole by ESO  This image indicates the location of the newly discovered binary star D9, which is orbiting Sagittarius A*, the supermassive black hole at the center of our galaxy. It is the first star pair ever found near a supermassive black hole. The cut-out shows the binary system as detected by the SINFONI spectrograph on ESO's Very Large Telescope. While the two stars cannot be discerned separately in this image, the binary nature of D9 was revealed by the spectra captured by SINFONI over several years. These spectra showed that the light emitted by hydrogen gas around D9 oscillates periodically towards red and blue wavelengths as the two stars orbit each other. Credit: ESO/F. Peißker et al., S. Guisard An international team of researchers has detected a binary star orbiting close to Sagittarius A*, the supermassive black hole at the center of our galaxy. It is the first time a stellar pair has been found in the vicinity of a supermassive black hole. The discovery, based on data collected by the European Southern Observatory's Very Large Telescope (ESO's VLT), helps us understand how stars survive in environments with extreme gravity, and could pave the way for the detection of planets close to Sagittarius A*. "Black holes are not as destructive as we thought," says Florian Peißker, a researcher at the University of Cologne, Germany, and lead author of the study published in Nature Communications. Binary stars, pairs of stars orbiting each other, are very common in the universe, but they had never before been found near a supermassive black hole, where the intense gravity can make stellar systems unstable. This new discovery shows that some binaries can briefly thrive, even under destructive conditions. D9, as the newly discovered binary star is called, was detected just in time: it is estimated to be only 2.7 million years old, and the strong gravitational force of the nearby black hole will probably cause it to merge into a single star within just one million years, a very narrow timespan for such a young system. "This provides only a brief window on cosmic timescales to observe such a binary system—and we succeeded," explains co-author Emma Bordier, a researcher also at the University of Cologne and a former student at ESO. For many years, scientists also thought that the extreme environment near a supermassive black hole prevented new stars from forming there. Several young stars found in close proximity to Sagittarius A* have disproved this assumption. The discovery of the young binary star now shows that even stellar pairs have the potential to form in these harsh conditions. "The D9 system shows clear signs of the presence of gas and dust around the stars, which suggests that it could be a very young stellar system that must have formed in the vicinity of the supermassive black hole," explains co-author Michal Zajaček, a researcher at Masaryk University, Czechia, and the University of Cologne. The newly discovered binary was found in a dense cluster of stars and other objects orbiting Sagittarius A*, called the S cluster. Most enigmatic in this cluster are the G objects, which behave like stars but look like clouds of gas and dust. It was during their observations of these mysterious objects that the team found a surprising pattern in D9. The data obtained with the VLT's ERIS instrument, combined with archival data from the SINFONI instrument, revealed recurring variations in the velocity of the star, indicating D9 was actually two stars orbiting each other. "I thought that my analysis was wrong," Peißker says, "but the spectroscopic pattern covered about 15 years, and it was clear this detection is indeed the first binary observed in the S cluster." The results shed new light on what the mysterious G objects could be. The team proposes that they might actually be a combination of binary stars that have not yet merged and the leftover material from already merged stars. The precise nature of many of the objects orbiting Sagittarius A*, as well as how they could have formed so close to the supermassive black hole, remain a mystery. But soon, the GRAVITY+ upgrade to the VLT Interferometer and the METIS instrument on ESO's Extremely Large Telescope (ELT), under construction in Chile, could change this. Both facilities will allow the team to carry out even more detailed observations of the Galactic center, revealing the nature of known objects and undoubtedly uncovering more binary stars and young systems. "Our discovery lets us speculate about the presence of planets, since these are often formed around young stars. It seems plausible that the detection of planets in the Galactic center is just a matter of time," concludes Peißker. | |
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| vtwin88cubePosted at 2024-12-18 02:16:14(6Days ago) Report Permalink URL | ||||
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|  IMAX.Hubble.2010.720p.BDRip.x264.AAC Subs: English French Spanish Genre: Space, Science, Documentary Length: 43:00 IMDB: https://www.imdb.com/title/tt1433813 Director: Toni Myers Plot: Hubble (also known as Hubble 3D, IMAX: Hubble, or IMAX: Hubble 3D) is a 2010 American documentary film about Space Shuttle missions to repair and upgrade the Hubble Space Telescope. It is narrated by the actor Leonardo DiCaprio.
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| Jase1Posted at 2024-12-24 12:36:15(18Mins ago) Report Permalink URL | ||
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|  This new image of star cluster NGC 602, released on Dec. 17, 2024, combines data from NASA’s Chandra X-ray Observatory with a previously released image from the agency’s James Webb Space Telescope. Webb data provide the ring-like outline of the “wreath,” while X-rays from Chandra (red) show young, massive stars that are illuminating the wreath, sending high-energy light into interstellar space. NGC 602 lies on the outskirts of the Small Magellanic Cloud, which is one of the closest galaxies to the Milky Way, about 200,000 light-years from Earth. Credit - ESA/Webb, NASA & CSA, P. Zeidler | |
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