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China’s Zhurong rover was equipped with a ground-penetrating radar system‚ allowing it to peer beneath Mars’s surface. Researchers have announced new results from the scans of Zhurong’s landing site in Utopia Planitia‚ saying they identified irregular polygonal wedges located at a depth of about 35 meters all along the robot’s journey. The objects measure from centimeters to tens of meters across. The scientists believe the buried polygons resulted from freeze-thaw cycles on Mars billions of years ago‚ but they could also be volcanic‚ from cooling lava flows. A wireless camera took this ‘group photo’ of China’s Tianwen-1 lander and rover on Mars’ surface. Credit: Chinese Space Agency The Zhurong rover landed on Mars on May 15‚ 2021‚ making China the second country ever to successfully land a rover on Mars. The cute rover‚ named after a Chinese god of fire‚ explored its landing site‚ sent back pictures — including a selfie with its lander‚ taken by a remote camera – studied the topography of Mars‚ and conducted measurements with its ground penetrating radar (GPR) instrument. Zhurong had a primary mission lifetime of three Earth months but it operated successfully for just over one Earth year before entering a planned hibernation. However‚ the rover has not been heard from since May of 2022. Researchers from the Institute of Geology and Geophysics under the Chinese Academy of Sciences who worked with Zhurong’s data said the GPR provides an important complement to orbital radar explorations from missions such as ESA’s Mars Express and China’s own Tianwen-1 orbiter. They said in-situ GPR surveying can provide critical local details of shallow structures and composition within approximately 100-meter depths along the rover’s traverse. a‚ Topographic map of Utopia Planitia‚ showing the landing sites of the Zhurong rover‚ the Viking 2 lander and the Perseverance rover. The ?4?km elevation contour is shown. Four local regions (c–f) with polygonal terrain are marked with white squares. b‚ The Zhurong rover traverse from Sol 11 through Sol 113 (HiRISE image: ESP_073225_2055). Green segments denote the wedges of buried polygons recognized from Fig. 2 (P1–P16). Purple segments denote the interiors of the polygons. c–f‚ Four representative HiRISE images of polygons in Utopia Planitia whose locations are marked in a: PSP_002202_2250 (c)‚ PSP_006962_2215 (d)‚ PSP_002162_2260 (e) and PSP_003177_2275 (f). Note the range of spatial scales for the sizes of the polygons. The average diameters of polygons shown in c–f are calculated in Extended Data Fig. 6. Credit for HiRISE images: NASA/JPL/University of Arizona. Utopia Planitia is a large plain within Utopia‚ the largest recognized impact basin on Mars (also in the Solar System) with an estimated diameter of 3‚300 km. In total‚ the rover traveled 1‚921 meters during its lifetime. The researchers‚ led by Lei Zhang‚ wrote in their paper published in Nature‚ that the rover’s radar detected sixteen polygonal wedges within about 1.2?kilometers distance‚ which suggests a wide distribution of similar terrain under Utopia Planitia. These detected features probably formed 3.7 – 2.9 billion years ago during the Late Hesperian–Early Amazonian epochs on Mars‚ “possibly with the cessation of an ancient wet environment. The palaeo-polygonal terrain‚ either with or without being eroded‚ was subsequently buried” by later geological processes. Schematic model of the polygonal terrain formation process at the Zhurong landing site. a‚ The origination of thermal contraction cracking on the surface. b‚ The formation of cracks infilled by water ice or soil material‚ causing three types of polygonal terrain (ice-wedge‚ composite-wedge and sand-wedge polygons). c‚ The stabilization of the surface polygonal terrain in the Late Hesperian–Early Amazonian‚ possibly with the cessation of an ancient wet environment. d‚ The palaeo-polygonal terrain‚ either with or without being eroded‚ was subsequently buried by deposition of the covering materials in the Amazonian. The Mars surface image was acquired by the Navigation and Terrain Camera (NaTeCam). Credit: Zhang et al. While polygon-type terrain has been seen across several areas of Mars from many previous missions‚ this is the first time there has been indications of buried polygon features. The buried polygonal terrain requires a cold environment‚ the researchers wrote‚ that might be related to water/ice freeze–thaw processes in southern Utopia Planitia on early Mars. “The possible presence of water and ice required for the freeze–thaw process in the wedges may have come from cryogenic suction-induced moisture migration from an underground aquifer on Mars‚ snowfall from the air or vapor diffusion for pore ice deposition‚” the paper explains. Earlier research from Zhurong’s radar data indicated that multiple floods during that same time frame created several layers beneath the surface of Utopia Planitia. While the new paper indicates that the most likely possible formation mechanisms would be soil contraction from wet sediments that dried‚ producing mud-cracks‚ however‚ contraction from cooling lava could have also produced thermal contraction cracking. Either way‚ they note that a huge change in Mars’ climate was responsible for the polygon’s formation. “The subsurface structure with the covering materials overlying the buried palaeo-polygonal terrain suggests that there was a notable palaeoclimatic transformation some time thereafter‚” the researchers wrote. “The contrast above and below about-35-meter depth represented a notable transformation of water activity or thermal conditions in ancient Martian time‚ implying that there was a climatic upheaval at low-to-mid latitudes.” The post There are Myterious Polygons Beneath the Surface of Mars appeared first on Universe Today.

Astronomers have imaged dozens of protoplanetary discs around Milky Way stars‚ seeing them at all stages of formation. Now‚ one of these discs has been found for the first time — excitingly — in another galaxy. The discovery was made using the Atacama Large Millimeter/Submillimeter Array (ALMA) in Chile along with the ‚ which detected the telltale signature of a spinning disc around a massive star in the Large Magellanic Cloud‚ located 160‚000 light-years away. “When I first saw evidence for a rotating structure in the ALMA data I could not believe that we had detected the first extragalactic accretion disc‚ it was a special moment‚” said Anna McLeod‚ an associate professor at Durham University in the UK and lead author of the study published in Nature. “We know discs are vital to forming stars and planets in our galaxy‚ and here‚ for the first time‚ we’re seeing direct evidence for this in another galaxy.” McLeod and her fellow researchers were doing a follow-up study on a system named HH 1177‚ which was located deep inside a gas cloud in the Large Magellanic Cloud LMC). In 2019‚ the researchers reported that in using the Very Large Telescope‚ they observed a jet emitted by a fledgling but massive star with a mass 12 times greater than our Sun. This was the first time such a jet has been observed in visible light outside the Milky Way‚ as they are usually obscured by their dusty surroundings. However‚ the relatively dust-free environment of the LMC allowed for HH 1177 to be observed at visible wavelengths. At nearly 33 light-years in length‚ it is one of the longest such jets ever observed. This dazzling region of newly-forming stars in the Large Magellanic Cloud (LMC) was captured by the Multi Unit Spectroscopic Explorer instrument on ESO’s Very Large Telescope. The relatively small amount of dust in the LMC and MUSE’s acute vision allowed intricate details of the region to be picked out in visible light. Credit: ESO‚ A McLeod et al. “We discovered a jet being launched from this young massive star‚ and its presence is a signpost for ongoing disc accretion‚” McLeod said in an ESO press release. But to confirm that such a disc was indeed present‚ the team needed to measure the movement of the dense gas around the star. The gas motion indicated that there is a radial flow of material falling onto a central disk-like structure. In their new observations‚ the team found that the disk exhibits signs of Keplerian rotation – which is a disk of material that obey’s Kepler’s laws of motion due to the dominance of a massive body at its center. Their observations revealed that “the rotating toroid [was] feeding an accretion disk and thus the growth of the central star‚” the McLeod and team wrote in their paper. “The system is in almost all aspects comparable to Milky Way high-mass YSOs (young stellar objects) accreting gas from a Keplerian disk. As matter is pulled towards a growing star‚ it cannot fall directly onto it; instead‚ it flattens into a spinning disc around the star. Closer to the center‚ the disc rotates faster‚ and this difference in speed is the clear evidence to show astronomers an accretion disc is present. “The frequency of light changes depending on how fast the gas emitting the light is moving towards or away from us‚” said Jonathan Henshaw‚ a research fellow at Liverpool John Moores University in the UK‚ and co-author of the study‚ in the ESO press release. “This is precisely the same phenomenon that occurs when the pitch of an ambulance siren changes as it passes you and the frequency of the sound goes from higher to lower.” Massive stars like HH 1177 live fast and die hard. In the Milky Way‚ stars like this are challenging to observe because they are often clouded from view by the dusty material from which they form — which also obscures the disc that might be shaping around them. “They form in heavily embedded regions full of gas and dust‚ such that the accretion phase typically occurs before the star has time to become exposed due to stellar feedback‚ whether internal or external‚” the team wrote in their paper. “The primary reason for the lack of observations of extragalactic accretion disks around forming stars has been the limited spatial resolution of both ground- and space-based observatories.” But the Large Magellanic Cloud is fundamentally different from because the stars that form there have a lower dust content than in the Milky Way. Because of that HH 1177 is no longer cloaked in its early dust cloud‚ providing astronomers an unobstructed view‚ even though it is so far away. The researchers said the instruments on ALMA enables the high-sensitivity and high-angular-resolution observations needed to detect and resolve rotating circumstellar gas in the LMC. “We are in an era of rapid technological advancement when it comes to astronomical facilities‚” McLeod says. “Being able to study how stars form at such incredible distances and in a different galaxy is very exciting.” The post A Protoplanetary Disc Has Been Found… in Another Galaxy! appeared first on Universe Today.

Chinese and Indian astronomers were the first to measure Earth’s axial tilt accurately‚ and they did it about 3‚000 years ago. Their measurements were remarkably accurate: in 1120 BC‚ Chinese astronomers pegged the Earth’s axial tilt at 24 degrees. Now we know that all of the planets in the Solar System‚ with the exception of Mercury‚ have some tilt. While astronomers have puzzled over why our Solar System’s planets are tilted‚ it turns out it’s rather normal. Now that astronomers have observed so many other solar systems‚ they’ve learned that axial tilt is to be expected‚ even in so-called “pristine” solar systems. Pristine refers to the precise mathematical relationship between planets. New research in The Astronomical Journal explains why some axial tilt is to be expected. It’s titled “Evidence for Low-level Dynamical Excitation in Near-resonant Exoplanet Systems.” The lead author is Malena Rice‚ an assistant professor of astronomy at Yale’s Faculty of Arts and Sciences. The orbital resonance concept is at the heart of this research. As planets orbit a star‚ they can exert regular and periodic gravitational influence on one another. When they do‚ astronomers say they’re in resonance with one another. It also happens in moon systems around planets with many moons. Some resonant systems can be self-stabilizing‚ while others can become unstabilized over time. This video does a good job of illustrating orbital resonance using three of Jupiter’s moons. Early in a solar system’s history‚ planets are more likely to be in resonance with one another. “This type of configuration‚ where one planet’s orbit is precisely ordered with another in an exact integer ratio of orbital periods‚ is likely common to find in a solar system early in its development‚” said Rice. “It’s a gorgeous configuration — but only a small percentage of systems retain it.” “Given that near-resonant systems have likely experienced minimal dynamical disruptions‚ the spin-orbit orientations of these systems inform the typical outcomes of quiescent planet formation‚ as well as the primordial stellar obliquity distribution‚” the authors write in their research. The spin-orbit orientation is the tilt of companion planets’ orbits relative to the host star’s spin axis. What that boils down to is that in a system that’s suffered few disruptions‚ like migrating planets‚ for example‚ the spin-orbit and axial tilt of the planets in the system should be largely unchanged from the time of formation. But the problem is astronomers haven’t rigorously measured the spin-orbit orientations of near-resonant systems. “To date‚ only a handful of near-resonant systems have had spin-orbit angles measured to characterize the tilts of their constituent planetary orbits‚” the authors explain in their research. In this work‚ the researchers started out by examining a warm Jupiter named TOI-2202 b. It’s a near-resonant planet that’s only slightly less massive than Jupiter. It orbits a K-type star about 770 light-years away. TOI-2202 b is tight to its star‚ only 0.09564 AU away‚ and it completes an orbit in only 11.9 days. For comparison‚ Mercury is 0.387098 AU away from the Sun. TOI-2202 b is in a pristine solar system‚ and it’s in a 2:1 mean-motion resonance with another planet further from the star. The researchers compared it to archival data and new observations of the exoplanet from multiple telescopes. They arrived at a spin-orbit angle of about 31 degrees. Then they compared that to the full census of other similar planets in pristine systems found in NASA’s Exoplanet Archive. “To place this measurement into context‚ we examined the full set of transiting exoplanet systems with (1) a sky-projected spin-orbit measurement and (2) evidence that the transiting planet lies near a low-order mean-motion resonance with a neighbouring companion‚” the authors explain in their research. They found that planets in these pristine systems exhibit a typical spin-orbit angle of around 20 degrees. So even “quiet” solar systems have axial tilt. TOI-2202 b was one of the most strongly tilted planets in the sample. “The measured spin-orbit angle of TOI-2202 b‚ together with the full census of spin-orbit measurements for near-resonant exoplanets‚ indicates that even quiescently formed systems may experience low-level dynamical excitation that produces some dispersion in their spin-orbit orientations‚” the authors write. This is an artist’s illustration of TOI-2202 b. Image Credit: NASA This told the researchers that our Solar System’s tilted planets are the norm rather than an oddball outlier. “It’s reassuring‚” Rice said. “It tells us that we’re not a super-weird solar system. This is really like looking at ourselves in a funhouse mirror and seeing how we fit into the bigger picture of the universe.” Our Solar System does contain one oddball‚ though: Uranus. Uranus’s tilt angle is 97.77 degrees‚ nearly parallel to the Solar System’s plane. Astronomers aren’t certain‚ but a collision with an Earth-sized protoplanet in the Solar System’s early days is likely the cause. One of Rice’s research areas concerns hot Jupiters and why they exhibit such pronounced axial tilts. “I’m trying to figure out why systems with hot Jupiters have such extremely tilted orbits‚” Rice said. “When did they get tilted? Can they just be born that way? To find that out‚ I first need to find out what types of systems are not so dramatically tilted.” That search continues. The post It Doesn’t Take Much to Get Tilted Planets appeared first on Universe Today.

Back to the drawing board?

Hall says his bandmate tried to "ambush" him with a catalog sale in an attempt to "cause me the maximum amount of harm." Continue reading…

Former Arkansas Governor Mike Huckabee said that an impeachment vote on United States President Joe Biden would be a “political disaster” for House GOP members.

Washington‚ D.C.‚ is paying $270‚000 to touch up the paint job on the “Black Lives Matter Plaza” amid rising crime rates.