Two colossal, ultra-hot rock formations, positioned 2,900 kilometers beneath the Earth’s surface in Africa and the Pacific Ocean, have influenced Earth’s magnetic field for millions of years, according to groundbreaking research led by Professor Andy Biggin from the University of Liverpool.
Giant superheated solid masses at the Earth’s mantle base impact the liquid outer core. Image credit: Biggin et al., doi: 10.1038/s41561-025-01910-1.
Measuring ancient magnetic fields and simulating their generation presents significant technical challenges.
To explore these deep Earth features, Professor Biggin and his team used paleomagnetic data in conjunction with advanced Earth Dynamo simulations. The flow of liquid iron in the outer core generates Earth’s magnetic field, akin to a wind turbine producing electricity.
Numerical models reconstructed critical insights about magnetic field behavior over the past 265 million years.
Even with supercomputers, conducting these long-term simulations poses enormous computational challenges.
The findings showed that temperature at the upper layer of the outer core is not uniform.
Instead, localized hot areas are accompanied by continent-sized rock structures exhibiting significant thermal contrasts.
Some regions of the magnetic field were found to remain relatively stable over hundreds of millions of years, while others displayed considerable changes over time.
“These results indicate pronounced temperature variations in the rocky mantle just above the core, suggesting that beneath hotter regions, liquid iron in the core may be stagnant, rather than flowing intensely as observed beneath colder areas,” Professor Biggin stated.
“Gaining such insights into the deep Earth over extensive timescales enhances the case for utilizing ancient magnetic records to comprehend both the dynamic evolution and stable properties of deep Earth.”
“These discoveries also bear significant implications for understanding ancient continents, including the formation and breakup of Pangea, and could help address long-standing uncertainties in ancient climate studies, paleontology, and natural resource formation.”
“It has been hypothesized that, on average, Earth’s magnetic field acts as a perfect bar magnet aligned with the planet’s rotation axis in these regions.”
“Our findings suggest that this may not be entirely accurate.”
This study is published in today’s edition of Nature Earth Science.
_____
AJ Biggin et al. Inhomogeneities in the mantle influenced Earth’s ancient magnetic field. Nature Earth Science published online on February 3, 2026. doi: 10.1038/s41561-025-01910-1
Recent high-resolution findings from ESA’s Solar Orbiter mission provide groundbreaking insights into solar flares. These explosive events are triggered by cascading magnetic reconnection processes, releasing immense energy and “raining down” plasma clumps into the Sun’s atmosphere.
Detailed overview of M-class solar flares as observed by ESA’s solar probes. Image credit: ESA / Solar Orbiter / Chitta et al., doi: 10.1051/0004-6361/202557253.
Solar flares are powerful explosions originating from the Sun.
These dramatic events occur when energy stored in entangled magnetic fields is suddenly unleashed through a process known as “magnetic reconnection.”
In mere minutes, intersecting magnetic field lines disconnect and reconnect, leading to a rapid rise in temperature and accelerating millions of degrees of plasma and high-energy particles, potentially resulting in solar flares.
The most intense flares can initiate a cascade of reactions, causing magnetic storms on Earth and potentially disrupting radio communications. Hence, monitoring and understanding these flares is crucial.
However, the mechanisms behind such swift energy release remain largely enigmatic.
An exceptional series of observations from the Solar Orbiter’s four instruments has finally provided clarity. This mission, with its comprehensive approach, offers the most detailed perspective on solar flares to date.
The Solar Orbiter’s Extreme Ultraviolet Imager (EUI) captured high-resolution images of features just hundreds of kilometers across in the Sun’s outer atmosphere (corona), recording changes every two seconds.
Three other instruments—SPICE, STIX, and PHI—examined various depth and temperature regions, from the corona to the Sun’s visible surface, or photosphere.
“We were fortunate to witness this massive flare precursor in such exquisite detail,” said Dr. Pradeep Chitta, an astronomer at the Max Planck Institute for Solar System Research.
“Such detailed and frequent observations of flares are rarely possible due to the limited observation window and the significant data storage required.”
“We were in the right place at the right time to capture these intricate details of the flare.”
Solar Orbiter observations have revealed an intricate view of the central engine during the preflare and shock stages of a solar flare as a magnetic avalanche.
“Even prior to the major flare event, ribbon-like features rapidly traversed the Sun’s atmosphere,” Dr. Chitta noted.
“The flow of these ‘rainy plasma blobs’ indicates increasing energy buildup, intensifying as the flare progresses.”
“This rain of plasma will continue for a while even after the flare diminishes.”
“This marks the first time we’ve observed such a level of spatial and temporal detail in the solar corona.”
“We did not anticipate such high-energy particles emerging from the avalanche process.”
“There is still much to explore regarding this phenomenon, but future missions equipped with high-resolution X-ray imaging will further our understanding.”
“This is one of Solar Orbiter’s most thrilling achievements thus far,” stated Dr. Miho Jamby, ESA’s Solar Orbiter Collaborative Project Scientist.
“The Solar Orbiter’s observations unveil the flare’s central engine and underscore the significant role of an avalanche-like magnetic energy release mechanism.”
There is a compelling prospect of whether this mechanism is universal across all flares and in other flaring stars.
Results can be found in the journal Astronomy and Astrophysics.
_____
LP Citta et al. 2026. Magnetic avalanches as the central engine driving solar flares. A&A 705, A113; doi: 10.1051/0004-6361/202557253
Utilizing magnetic fields to maneuver satellites could significantly enhance the longevity of space exploration missions and reduce the risk of collisions between spacecraft.
Currently, most space missions and artificial satellites depend on propellant for movement in space, which limits their operational lifetimes due to fuel depletion. An innovative alternative, known as electromagnetic formation flight (EMFF), employs renewable energy sources like solar panels to power onboard electromagnetic coils. These coils generate magnetic fields that can theoretically steer spacecraft through interactions with similar fields from adjacent satellites.
However, researchers have faced challenges with EMFF due to a phenomenon called electromagnetic coupling. The magnetic field from one satellite affects not just nearby satellites but all satellites in proximity, complicating coordinated movement among multiple objects.
A research team at the University of Kentucky has proposed a promising solution through a method called alternating magnetic field forcing (AMFF).
This technique enables two satellites to communicate and control each other’s trajectories without disrupting a third satellite. This is achieved by utilizing distinct interaction frequencies, allowing two satellites to coordinate on one frequency while maintaining communication with others on different frequencies.
The AMFF concept has been successfully tested on Earth instead of in space. The three satellites were positioned on specialized linear rails employing high-pressure air to create a low-friction environment. With the integrated laser ranging module, the satellites achieved precise travel distances and effective interactions as defined by the researchers.
The project team did not respond to interview requests. However, Alvar Saenz Otero, a researcher at the University of Washington, noted that this paper represents a significant advancement in a long-standing research area. “The complexity of a formation flight system increases significantly when transitioning from two to three satellites,” he explains.
Yet, Otero expresses skepticism about the immediate application of this technology for low-Earth orbit satellites, such as massive constellations like Starlink. “Our work on EMFF has primarily focused on deep space operations,” he adds.
Earth’s atmosphere can impact the frequencies utilized for EMFF or AMFF, introducing interference that complicates satellite control, he notes.
While it is currently feasible for three units to fly together and utilize magnetic fields for navigation, scaling this approach to manage thousands of satellites poses a formidable challenge. “This is not applicable at the constellation level,” remarks Ray Sedwick from the University of Maryland.
“Employing superconducting magnetic coils significantly extends the operational range of EMFF, but numerous technical challenges remain,” Sedwick explains, indicating that large-scale magnetic motion might still be on the horizon.
Devices utilizing magnets may offer a more efficient method for removing kidney stones compared to traditional techniques, potentially reducing the necessity for repeated surgeries.
Kidney stones form when minerals in urine crystallize. If they become lodged in the kidneys or move into the ureters, the tubes connecting the kidneys to the bladder, they can lead to significant discomfort.
Current treatments often involve breaking the stones into smaller pieces through methods such as guiding a thin tube with a laser through the bladder into the ureters and kidneys, or applying ultrasound waves externally.
Surgeons typically extract these fragments individually using a wire basket that passes in and out of the urethra. This repetitive retrieval process can result in tissue damage. About 40% of the time, residual debris is left behind, particularly if small particles evade the basket, increasing the risk of additional stones.
Seeking alternatives, Joseph Liao and his team at Stanford University in California previously engineered a magnetic gel designed to coat stone debris and a magnetic wire to capture it in lab settings.
Recently, they implemented this method in a study involving four pigs. They introduced various fragments of human kidney stones into the pigs’ kidneys before injecting the magnetic gel. By utilizing a magnetic wire inserted through the urethra, the researchers managed to extract multiple stone fragments simultaneously, unlike the traditional wire basket method that retrieves them one at a time. “It’s like using a stick to fish out a snot filled with stone debris, allowing for the removal of significant amounts of stone fragments at once,” explained Liao.
This technique appears to cause less tissue damage than conventional methods since fewer invasive procedures are necessary. Unlike wire baskets, the magnetic device effectively captures debris of varying sizes, permitting thorough removal of all remnants from the kidney, as noted by Rio. This not only decreases the chance of new stones forming but also curtails the need for additional surgeries.
“This is a very promising method,” states Veronica Magdanz from the University of Waterloo, Canada, who was not involved in the research. “Any advancement that enhances the success rate of stone collection and facilitates the removal of more pieces at once is advantageous.”
None of the pigs exhibited any adverse reactions to the gel. “This is excellent news. It is non-toxic and harmless,” Magdanz remarked. After refining the technique through further pig studies, Rio and his team aim to begin human trials within approximately a year.
This stream of gas transports material from the clouds surrounding the star-forming area within Perseus directly into an emerging binary star system known as SVS 13A.
Artist’s impression of the SVS 13A system. Image credit: NSF/AUI/NSF’s NRAO/P.Vosteen.
Stars are formed from clouds of gas and dust, and recent observations indicate that the process of star formation is far more dynamic than previously understood.
New findings from the Atacama Large Millimeter/Submillimeter Array (ALMA) reveal both dust and molecules swirling around the SVS 13A system. This data shows how the magnetic field not only permeates these stellar nurseries but actively directs the flow of matter, offering a preferred path for gas to accumulate in the disk where new stars and planets arise.
“Visualize a garden hose, but instead of water, it smoothly channels materials for star formation through intricate pathways carved by unseen forces,” explains Dr. Paulo Cortes, an astronomer at the NSF National Radio Astronomy Observatory and the joint ALMA telescope.
“This perspective from ALMA observations presents channels of gas known as subalfvénic streamers, regulated by spiral magnetic field lines.”
“This new data provides an insightful glimpse into the star formation process.”
“These streamers illustrate how magnetic fields can influence star formation by managing material influx, akin to a private highway facilitating car travel.”
ALMA’s images and findings uncover two spiral arms of dust encircling the star, with gas streams closely mirroring the same trajectory.
This remarkable configuration implies that the gas within the streamer is traversing at a slower pace than previously believed, reinforcing the concept of a magnetized channel rather than a chaotic, collapsing cloud.
The presence of such streamers, linking clouds to disks and supplying them with material in a managed fashion, indicates that both gravity and magnetism are crucial in the formation of stars and the shaping of potential planetary bodies around them.
This groundbreaking result signifies the first instance where astronomers have directly mapped both a streamer and its associated magnetic field in a single observation.
“Subalfvenic streamers indicate a fresh role for magnetic fields amidst gravitational dominance, acting as ‘guides’ to assist the descent of material from the outer envelope to the disk,” the astronomers remarked.
Upcoming findings are detailed in a paper in the Astrophysics Journal Letter.
_____
PC Cortez et al. 2025. First results from ALPPS: SVS 13A subalfvenic streamer. APJL 992, L31; doi: 10.3847/2041-8213/ae0c04
Materials resembling magnets exhibit internal spirals that can solely be controlled with circularly polarized lasers.
Andrew Ostrovsky/iStockphoto/Getty Images
Scientists have successfully regulated the behavior of a previously elusive material, akin to magnetism, which may eventually lead to improved hard drives.
When a bar magnet is introduced to a magnetic field, it rotates due to that influence. However, materials characterized by a property called strong axis remain stationary under all known magnetic fields. Recently, Zeng Zhiyang and his team at the Max Planck Institute for the Structure and Mechanics of Matter in Germany discovered a method to manipulate strong-axis properties using lasers.
A conventional magnetic material is often thought of as a collection of many small bar magnets. Zeng explains that for strong-axis materials, it is more accurate to envision a group of dipoles (two opposing charges separated by a small distance) swirling in a minor spiral. He and his team realized they could control these vortices with laser pulses containing a specific swirl.
The researchers adjusted the laser to emit circularly polarized light. Upon striking a strong-axis material (specifically a compound made of rubidium, iron, molybdenum, and oxygen), it induced rotation in the material’s atoms, altering the dipole’s direction of motion.
Team member Michael Forst from the Max Planck Institute for Structure and Mechanics of Matter remarked that while it has been established that light can effectively control materials—transforming conductors into insulators and vice versa—tailoring light’s properties for material control has presented a significant technical challenge.
“This serves as a strong proof of concept,” notes Theo Rasing at Radboud University in the Netherlands. He adds that this material adds to the growing array of options for constructing more efficient and stable memory devices, such as hard drives that store information in electromagnetic charge patterns.
However, the current experiments necessitate cooling the material to approximately -70°C.°C (-94°F). Additionally, because the team’s laser was relatively large, Forst indicates that more development is required before a practical device can realistically be constructed.
google’s Pixel SuperPhone returns, featuring enhanced battery life, rapid charging, magnetic accessories, and cutting-edge AI tools, aiming to challenge the dominance of Apple and Samsung in the mobile market.
The Pixel 10 Pro XL is Google’s largest smartphone, and it ranks among the biggest available in Europe and the US. Priced at £1,199 (€1,299/$1,199/$1,999), it sits at the pinnacle of the Pixel 10 Pro range, just below the forthcoming folding Pixel 10 Pro Fold, and competes head-on with Apple’s iPhone 17 Pro Max and Samsung’s Galaxy S25 Ultra.
Similar in size to the previous generation, the 10 Pro XL boasts a slight increase in weight of 11g. It’s a sizable and hefty device that usually requires two hands for operation and benefits from accessories like grips or handles.
The device features a magnetic ring that allows for various Qi2 or MagSafe accessories, including grips, car mounts, wallets, stands, batteries, and more. Photo: Samuel Gibbs/The Guardian
It sports a large, bright OLED display that offers a superb viewing experience for TV shows and movies. The rear integrates QI2.2 wireless charging and magnetic accessory support, positioning it as one of the few smartphones able to charge at up to 25W with the latest wireless chargers.
The 10 Pro XL carries the same Google Tensor G5 chip found in the entire Pixel 10 series, providing smooth and responsive performance. While it handles gaming adequately, those seeking top-tier graphics and frame rates may prefer competitors using Qualcomm’s premium Snapdragon processors, such as the S25 Ultra.
With the largest battery among the Pixels, the 10 Pro XL offers impressive longevity. It matches its predecessor, providing roughly 52 hours of use through a combination of Wi-Fi and 5G. Users can expect it to last through even the most demanding days, typically requiring charging every other day.
Charging is quick, taking under 90 minutes via cable and about 2 hours via a QI2 25W wireless charger. See the Ugreen Magflow 2-in-1 (left) or Belkin Ultracharge Pro (right) for options. Photo: Samuel Gibbs/The Guardian
Connectivity: 5G, eSIM, Wi-Fi 7, UWB, NFC, Bluetooth 6, GNSS
Water Resistance: IP68 (1.5m for 30 minutes)
Size: 162.8 x 76.6 x 8.5mm
Weight: 232g
Android 16 with AI
Magic Cue is among the most advanced AI features, working silently in the background to provide useful, timely information. Photo: Samuel Gibbs/The Guardian
The 10 Pro XL operates on Android 16 software, enriched with AI capabilities similar to the 10 Pro, delivering one of the most comprehensive and sophisticated user experiences available. Google will offer updates until 2032.
Gemini Chatbot is integrated system-wide, complemented by a standalone app that visually displays screen content. The standout new feature, Magic Cue, operates in the background, proactively showcasing data from calendars, emails, chats, and other Google apps as needed. Whether providing location details when a friend texts about dinner or displaying an order confirmation when a recognized business calls, it seamlessly integrates with various Google and select third-party apps, although it currently does not support popular messaging apps like WhatsApp.
Moreover, the 10 Pro XL includes a one-year subscription to Google AI Pro, granting access to Google’s more powerful Gemini models and 2TB of cloud storage for photos, files, and emails (valued at £19 per month).
Camera
With the 10 Pro XL, you’re likely to capture stunning photos in various conditions. Photo: Samuel Gibbs/The Guardian
The camera system on the larger Pixels mirrors that of the 10 Pro, meaning the choice lies in the size rather than the camera quality. Its 50MP main sensor, complemented by a 48MP ultra-wide and a 48MP 5x telephoto lens, provides some of the finest photo capabilities available. With a point-and-shoot approach on the Pro XL, you’re virtually guaranteed excellent results, irrespective of the conditions.
Additionally, several AI tools enhance the photography experience, including: Novel Camera Coach; Please Add Me that blends two photos to introduce the photographer into a group shot; and Best Take, which now operates automatically. By simply pressing the shutter button or combining multiple shots, you’re more likely to achieve group photos where everyone is looking at the camera.
Moreover, activating the Pro Res Zoom feature when exceeding a 30x zoom utilizes GenAI to restore details and clarity in images lost due to digital zoom. While results can vary, and the feature deactivates when it detects people, it often enhances blurry 100x zoom photos. It’s essential to note that this process interprets and reconstructs the image using AI, clearly indicated by the camera app. C2PA Content Credentials.
Overall, the Pixel camera system ranks among the best on the market, regardless of AI tool usage.
Sustainability
The fingerprint scanner at the bottom of the display is quick and accurate, enabling seamless unlocking. Photo: Samuel Gibbs/The Guardian
Battery longevity is rated to exceed 1,000 full charge cycles while maintaining at least 80% of its original capacity. Repairs can be conducted through Google, authorized third-party providers, or via self-repair using available parts and manuals.
The Pixel 10 Pro XL includes 29% recycled materials by weight, such as aluminum, cobalt, copper, glass, gold, plastic, rare earth elements, tungsten, and tin. The company is committed to minimizing its environmental impact, as indicated in their Environmental Report, and offers free recycling of old devices through their platform.
Price
The Google Pixel 10 Pro XL is priced at £1,199 (€1,299/$1,199/$1,999) and is available in four color options.
For context, the Pixel 10 is priced at £799, the Pixel 10 Pro at £999, and the Pixel 9a at £399. The Galaxy S25 Ultra retails for £1,249, while the iPhone 17 Pro Max is priced at £1,199.
Verdict
The Pixel 10 Pro XL epitomizes a superphone with significant size, price, and functionality. If you appreciate the features of Google’s 6.3-inch smartphone but desire larger dimensions, this model is the ideal choice.
The camera stands out as one of the best, the display is stunning, and the software, which integrates Google’s most advanced AI features, is superb. The introduction of QI2.2 support accelerates wireless charging while providing access to a range of magnetic accessories, such as grips that facilitate handling larger devices.
While the pixels exhibit responsiveness, they don’t represent a groundbreaking upgrade from last year’s 9 Pro XL. Particularly regarding raw gaming performance, they fall short compared to competitors like Samsung’s Galaxy S25 Ultra.
Pros: 7 years of software updates, 5x optical zoom and 10x AI zoom, excellent display, magic cues, stellar camera with impressive local AI capabilities, QI2.2 wireless charging and magnetic accessory support, exceptional battery life, great ergonomics, swift fingerprint and face recognition, and a one-year subscription to Google AI Pro.
Cons: High price point, large and heavy, reliance on face ID, insufficient raw performance, inconsistent battery performance, lack of physical SIM slot in US models, and not a significant enhancement over its predecessor.
Please note, the Pixel 10 Pro XL lacks a physical SIM slot in US versions, relying solely on eSIMs. Photo: Samuel Gibbs/The Guardian
Among the four fundamental forces in the universe, gravity often comes to mind when considering cosmic phenomena. This is quite logical, as gravity operates over vast distances, exerting its influence on massive objects, making it the most significant and far-reaching force. However, another essential force, known as electromagnetism, also plays a critical role in the study of space.
To begin with, all light is made up of electromagnetic radiation, which consists of oscillating electric and magnetic fields. This includes everything from radio waves to visible light and X-rays. Similar to Earth and the Sun, many celestial bodies are enveloped in magnetic fields. The Earth’s magnetic field serves as a shield against harmful radiation, while the solar magnetic field repels it. The generation of a magnetic field requires the movement of charged particles, such as protons and electrons. Consequently, a variety of objects, including entire galaxies, possess magnetic fields!
Researchers are aware that galaxies have magnetic fields, but it remains uncertain how various galaxies develop different magnetic intensities or how these fields influence their evolution over time. This investigation is further complicated by the fact that galaxies often exist in clusters. For instance, the Milky Way is surrounded by smaller galaxies known as satellites, which exert gravitational pull on each other and interfere with each other’s magnetic fields.
The research team explored how diverse environments in smaller galaxies affected the strength of their magnetic fields. They approached this by simulating the motion of materials within the galaxy as if they were liquids filled with striped particles. Two sets of simulations were conducted, the second of which also included the effects of high-energy particles known as cosmic rays.
In total, they simulated magnetic fields across 13 distinct scenarios, ranging from isolated galaxies with masses 10 billion times that of the Sun to those 10 trillion times greater, accompanied by up to 33 satellites. Each simulation commenced with galaxies exhibiting a magnetic field strength of 10-14 Gauss (g). For context, Earth’s magnetic field strength is about 0.3-0.6 g. The scenarios were evolved over 12 billion simulation years, allowing galaxies to interact, traverse space, and form stars, subsequently tracking the magnetic field strength in smaller galaxies.
Throughout the simulated timeline, the magnetic fields of all galaxies strengthened as star formation progressed. The birth of stars stirs the galactic matter, enhancing magnetic field strength and producing cosmic rays. Most galaxies concluded with magnetic fields ranging from 10-7 to 10-6 G, with larger galaxies typically achieving stronger fields. Interestingly, the researchers found that small galaxies passing in close proximity to larger companions exhibited stronger magnetic fields than equivalent isolated galaxies.
They monitored satellite galaxies over a series of simulations and discovered that, on average, magnetic field strength increased by 2-8 times as these galaxies approached their host. In extreme cases, the satellite’s magnetic field intensified by up to 15 times after nearing the host. In contrast, satellite galaxies that were more distant or had not yet approached their host did not show such significant increases in magnetic field strength.
The researchers interpret their findings to suggest that the more turbulent the interstellar medium (ISM) within a galaxy, the greater the strength of its magnetic field. Orbiting near a host galaxy tends to disturb the ISM of the satellite galaxy, rendering it more magnetic than a solitary small galaxy. Approaching a massive galaxy compresses the satellite, exposing it to magnetizing materials, and both interactions contribute to amplifying the magnetic field strength.
The team recommends that future studies utilize these results to inform radio and gamma-ray observations of galaxies, as these two segments of the electromagnetic spectrum can provide astronomers insights into the magnetic field properties of celestial bodies. They also caution that astronomers conducting simulations of isolated galaxies might yield skewed results since such a scenario does not accurately reflect the reality in which many galaxies are in proximity to companions.
Antimatter particles are fundamentally similar to their normal matter counterparts, differing primarily in their opposite charges and momentum.
Although extremely rare, physicists routinely generate antiparticles using particle accelerators. Additionally, anti-Dutters occur naturally in high-energy processes near the event horizons of black holes.
The question of how and why the universe is predominantly made up of normal matter remains unresolved.
Creating antimatter is a complex and costly endeavor. The European Institute of Particle Physics (CERN) plays a crucial role in this process. Using an anti-proton decelerator, a proton beam strikes a metal target, resulting in the generation of anti-protons.
However, this process only yields tens of thousands of particles.
One of the significant challenges with antimatter is that when it interacts with normal matter, it vanishes instantly, releasing energy. Therefore, the task of preventing its annihilation and storing it long-term poses a substantial technical hurdle.
Nonetheless, CERN engineers are working on methods to store and transport small amounts of anti-protons.
The challenge with antimatter is that it completely disappears upon contact with normal matter, releasing energy. – Image credits: Getty Images
To achieve this, researchers cool anti-protons to approximately -269ºC (-452.2°F) to nearly halt their motion. They then contain them in a high-vacuum enclosure to avoid contact with normal matter, using superconducting magnets to trap them.
This process must be managed while maintaining the capability to extract particles and introduce new ones into the enclosure.
Despite these challenges, CERN aims to develop “traps” capable of storing billions of anti-protons simultaneously. Recent techniques have been validated by transporting regular matter across the Swiss CERN facility.
With advancements in vacuum systems, antimatter storage and transport may soon become routine activities in the upcoming year.
This article addresses the question posed by Leighton Haas of Hamburg: “How is antimatter preserved?”
We welcome your inquiries! You can email us at Question @sciencefocus.com or reach us on Facebook, Twitter, or Instagram. Please include your name and location.
Explore our ultimateFun Factsfor more amazing science content!
A magnetor is a type of neutron star that boasts an extraordinarily strong magnetic field, approximately one times stronger than Earth’s magnetic field. These colossal magnetic fields are believed to be generated when rapidly rotating neutron stars are birthed from the collapse of a giant star’s core. Magnetars emit brilliant X-rays and display erratic patterns of activity, with bursts and flares releasing millions of times more energy than the Sun emits in just one second. Polarization measurements offer insights into magnetic fields and surface characteristics. This was the focus of astronomers using the NASA Imaging X-ray Polarization Explorer (IXPE) to study 1E 1841-045, a magnetor located within Supernova Remnant (SNR) KES 73, situated nearly 28,000 light years from Earth. The findings are published in the Astrophysics Journal Letter.
Impressions of Magneter artists. Image credit: NASA’s Goddard Space Flight Center/S. Wesinger.
Magnetors represent a category of young neutron stars. They are the remnants of giant stars that collapsed in on themselves at the end of their life cycles, resembling the mass of the Sun but compressed into a city-sized volume.
Neutron stars exemplify some of the most extreme physical conditions in the observable universe, offering a unique chance to investigate states that cannot be replicated in terrestrial laboratories.
The 1E 1841-045 magnetor was observed in an explosive state on August 21, 2024, by NASA’s Swift, Fermi, and other advanced telescopes.
The IXPE team has permitted several requests to pause scheduled observations of the telescope multiple times each year, redirecting focus to unique and unexpected celestial phenomena.
When 1E 1841-045 transitioned into this bright active phase, scientists chose to direct IXPE to capture the first polarization measurements of the magnetor’s flare.
Magnetors possess magnetic fields thousands of times stronger than most neutron stars, hosting the most powerful magnetic fields among known cosmic entities.
These extreme magnetic field fluctuations can lead to the emission of X-ray energies up to 1,000 times greater than usual for several weeks.
This heightened state is referred to as explosive activity, though the underlying mechanisms remain poorly understood.
IXPE’s X-ray polarization measurements may help unveil the mysteries behind these phenomena.
Polarized light carries information about the direction and orientation of emitted X-ray waves. A higher degree of polarization indicates that the X-ray waves are moving in harmony, akin to a tightly choreographed dance.
Studying the polarization characteristics of magnetors provides clues regarding the energy processes associated with observed photons and the direction and configuration of the magnetor’s magnetic field.
This diagram illustrates the IXPE measurements of X-ray polarized light emitted by 1E 1841-045. Image credit: Michela Rigoselli / Italian National Institute of Astrophysics.
IXPE results, supported by NASA’s Nustar and other telescope observations, indicate that X-ray emissions from 1E 1841-045 exhibit increased polarization at higher energy levels while maintaining a consistent emission direction.
This significant contribution to the high degree of polarization is attributed to the hard X-ray tail of 1E 1841-045, a highly energetic component of the magnetosphere responsible for the highest photon energies detected by IXPE.
Hard X-rays refer to X-rays characterized by shorter wavelengths and greater energy than soft X-rays.
While prevalent in magnetars, the processes that facilitate the generation of these high-energy X-ray photons remain largely enigmatic.
Despite several proposed theories explaining this emission, the high polarization associated with these hard X-rays currently offers additional clues to their origins.
“This unique observation enhances existing models that aim to explain magnetic hard X-ray emissions by elucidating the extensive synchronization seen among these hard X-ray photons,” remarked a student from George Washington University. First paper.
“This effectively demonstrates the power of polarization measurements in refining our understanding of the physics within a magnetar’s extreme environment.”
“It would be fascinating to observe 1E 1841-045 as it returns to its stable baseline state and to track the evolution of polarization,” added Dr. Michela Rigoselli, an astronomer at the National Institute of Astrophysics in Italy. Second paper.
____
Rachel Stewart et al. 2025. X-ray polarization of Magnetor 1E 1841-045. apjl 985, L35; doi: 10.3847/2041-8213/adbffa
Michela Rigoselli et al. 2025. IXPE detection of highly polarized X-rays from Magnetor 1E 1841-045. apjl 985, L34; doi: 10.3847/2041-8213/adbffb
Researchers from the Muon G-2 Experiment have unveiled their third measurement of the Muon magnetic anomaly. The conclusive results align with findings published in 2021 and 2023 but boast significantly improved precision at 127 parts per billion, surpassing the experimental goal for 140 people.
Muon particles traveling through lead in the cloud chamber. Image credit: Jino John 1996 / cc by-sa 4.0.
The Muon G-2 experiment investigates the wobble of a fundamental particle known as the Muon.
Muons resemble electrons but are roughly 200 times more massive. Like electrons, they exhibit quantum mechanical properties called spins, which can be interpreted as tiny internal magnets.
When subjected to an external magnetic field, these internal magnets wobble akin to the axis of a spinning top.
The precession speed of a magnetic field is influenced by the muon’s characteristics, captured numerically as the G-factor.
Theoretical physicists derive G-factors based on our current understanding of the universe’s fundamental mechanics, as outlined in the standard model of particle physics.
Nearly a century ago, G was anticipated to be 2; however, experimental measurements revealed minor deviations from this value, quantified as the Muon magnetic anomaly, Aμ, based on the formula (G-2)/2, giving the Muon G-2 experiment its name.
Muon magnetic anomalies encapsulate the effects of all standard model particles, enabling theoretical physicists to compute these contributions with remarkable precision.
Earlier measurements conducted at the Brookhaven National Laboratory during the 1990s and 2000s indicated potential discrepancies with the theoretical calculations of that era.
Disparities between experimental results and theoretical predictions could signal the existence of new physics.
In particular, physicists contemplated whether these discrepancies could stem from an undetected particle influencing the muon’s precession.
Consequently, physicists opted to enhance the Muon G-2 experiments to obtain more accurate measurements.
In 2013, Brookhaven’s magnetic storage ring was relocated from Long Island, New York, to Fermilab in Batavia, Illinois.
Following extensive upgrades and enhancements, the Fermilab Muon G-2 experiment launched on May 31, 2017.
Simultaneously, an international collaboration among theorists established the Muon G-2 theory initiative aimed at refining theoretical calculations.
In 2020, the Theoretical Initiative released updated and more precise standard model values informed by data from other experiments.
The differences between the experimental results continued to widen in 2021 as Fermilab announced the initial experimental results, corroborating Brookhaven’s findings with improved accuracy.
Simultaneously, new theoretical predictions emerged, relying significantly on computational capabilities.
This information closely aligned with experimental measurements and narrowed the existing discrepancies.
Recently, the Theoretical Initiative published a new set of predictions integrating results from various groups using novel calculation techniques.
This result remains in close agreement with experimental findings and diminishes the likelihood of new physics.
Nevertheless, theoretical endeavors will persist in addressing the disparities between data-driven and computational approaches.
The latest experimental values for the muon magnetic moment from Fermilab’s experiments are:
aμ =(g-2)/2 (Muon experiment) = 0.001 165 920 705
This final measurement is based on an analysis of data collected over the past three years, spanning 2021 to 2023, and is integrated with previously published datasets.
This has more than tripled the dataset size utilized in the second results from 2023, achieving the precision target set in 2012.
Moreover, it signifies the analysis of the highest quality data from the experiment.
As the second data collection run concluded, the Muon G-2 collaboration finalized adjustments and enhancements to the experiment, boosting muon beam quality and minimizing uncertainties.
“The extraordinary magnetic moment of the muon (G-2) is pivotal as it provides a sensitive test of the standard model of particle physics,” remarked Regina Lameika, associate director of high energy physics at the U.S. Department of Energy.
“This is an exhilarating result, and it’s fantastic to witness the experiment reach a definitive conclusion with precise measurements.”
“This highly anticipated outcome represents a remarkable achievement in accuracy and will hold the title of the most precise measurement of muon magnetic anomalies for the foreseeable future.”
“Despite recent theoretical challenges that have lessened the evidence for new physics in Muon G-2, this finding presents a robust benchmark for proposed extensions to the standard model of particle physics.”
“This is an incredibly exciting moment; not only did we meet our objectives, but we surpassed them, indicating that such precision measurements are challenging.”
“Thanks to Fermilab, the funding agencies, and the host lab, we accomplished our goals successfully.”
“For over a century, the G-2 has imparted crucial insights into the nature of reality,” stated Lawrence Gibbons, a professor at Cornell University.
“It’s thrilling to contribute accurate measurements that are likely to endure for a long time.”
“For decades, muon magnetic moments have served as a significant benchmark for the standard models,” noted Dr. Simon Kolody, a physicist at Argonne National Laboratory.
“The new experimental results illuminate this fundamental theory and establish a benchmark to guide new theoretical calculations.”
Since the Big Bang, the early universe has contained hydrogen, helium, and a minimal amount of lithium. Heavier elements, such as iron, were formed within stars. Yet, one of astrophysics’ greatest enigmas is how the first elements heavier than iron, like gold, were created and dispersed throughout the cosmos. A recent study by astronomers at Columbia University and other institutions suggests that a single flare from a magnetar could generate 27 equivalent masses of these elements simultaneously.
Impressions of Magnetar artists. Image credit: NASA’s Goddard Space Flight Center/S. Wesinger.
For decades, astronomers have theorized about the origins of some of nature’s heaviest elements, like gold, uranium, and platinum.
However, a fresh examination of older archival data indicates that up to 10% of these heavy elements in the Milky Way may originate from the emissions of highly magnetized neutron stars, known as magnetars.
“Until recently, astronomers largely overlooked the role that magnetars, the remnants of supernovae, might play in the formation of early galaxies,” remarked Todd Thompson, a professor at Ohio State University.
“Neutron stars are incredibly unique, dense objects known for their large size and strong magnetic fields. They are similar to black holes but not quite the same.”
The origin of heavy elements has long been a mystery, but scientists have understood that these elements can only form under specific conditions through a process known as the R process (or rapid neutron capture process).
This process was observed in 2017 when astronomers detected a collision between two super-dense neutron stars.
This event was captured using NASA telescopes and the LIGO gravitational wave observatory, providing the first direct evidence that heavy metals can be produced by celestial phenomena.
However, subsequent evidence suggests that neutron star collisions may not form heavy elements swiftly in the early universe, indicating that additional mechanisms might be necessary to account for all these elements.
Based on these insights, Professor Thompson and his colleagues realized that powerful magnetar flares could act as significant ejectors of heavy elements. This conclusion was validated by the observation of the SGR 1806-20 magnetar flare that occurred 20 years ago.
By analyzing this flare event, the researchers found that the radioactive decay of the newly formed elements aligns with theoretical predictions concerning the timing and energy released by magnetar flares after ejecting heavy R-process elements.
“This is the second time we’ve observed direct evidence of where these elements are produced, first linked to neutron star mergers,” stated Professor Brian Metzger from Columbia University.
“This marks a significant advancement in our understanding of heavy element production.”
“We are based at Columbia University,” mentioned Anildo Patel, a doctoral candidate at the institution.
The researchers also theorized that magnetar flares generate heavy cosmic rays and very fast particles, the origins of which remain unclear.
“I am always excited by new ideas about how systems and discoveries in space operate,” said Professor Thompson.
“That’s why seeing results like this is so thrilling.”
The team’s paper was published in The Astrophysical Journal Letters.
____
Anirudh Patel et al. 2025. Direct evidence for R-process nuclear synthesis in delayed MeV radiation from SGR 1806-20 magnetar giant flares. ApJL 984, L29; doi: 10.3847/2041-8213/ADC9B0
Recent measurements from NASA’s insight mission show that Mars’ core is less dense than previously believed planetary scientists. This shows that Mars has never developed a solid inner core at the earliest time in its history. in New research Published in the journal Geophysical Research BookResearchers at the University of Texas and elsewhere were hoping to understand the impact of this lack of a solid inner core.
Computer simulation of the unilateral magnetic field of early Mars. Image credits: Ankit Barik/Johns Hopkins University.
“Like Earth, Mars once had a strong magnetic field that protected the thick atmosphere from the solar wind,” said Dr. Chi Yang, a colleague at the University of Texas.
“But now only the magnetic imprint remains. But with a long, confused scientist, this imprint appears most strongly in the southern half of the red planet.”
The team’s new research will help explain the one-sided traces. We present evidence that the planet’s magnetic field covers only the southern half.
“The resulting biased magnetic field will match the traces we saw today,” Dr. Yang said.
“It will also make the Earth’s magnetic field that covers the entire Earth different from the Earth’s magnetic field.”
“If Mars’ inner core is liquid, a one-sided magnetic field can be generated.”
“The logic here is that it’s much easier to generate a hemispherical (one-sided) magnetic field because there is no solid inner core.”
“It could have influenced the ancient dynamos on Mars and perhaps could have maintained the atmosphere.”
In this study, researchers used computer simulations to model this scenario.
Until now, most early Mars studies relied on magnetic field models that gave the red planet an inner nucleus like Earth surrounded by solid, molten iron.
Scientists were urged to try to simulate a full liquid core after insights discovered that Mars’ core is made up of lighter than expected elements.
“That means there’s a very high chance that it’s melting because the core melts differently than Earth’s,” said Sabin Stanley, a professor at Johns Hopkins University.
“If Mars’ core was melting now, it would almost certainly have melted 4 billion years ago when it was known that Mars’ magnetic field was active.”
To test the idea, the author prepared an early Mars simulation with a liquid core and ran it dozens of times on a supercomputer.
With each run they made the northern half of the mantle planet a little hotter than the south.
Eventually, the temperature difference between the hotter mantle in the north and the colder mantle in the south began to escape from the core and only release at the southern tip of the planet.
The escape heat channeled in such a way was active enough to drive the dynamos and generate a powerful magnetic field focused on the Southern Hemisphere.
Planetary dynamos are self-supporting mechanisms that generate magnetic fields, usually through the movement of molten metal cores.
“We didn’t know if we’d explain the magnetic field, so it’s exciting to see that Mars’ interiors can create (single) hemispherical magnetic fields with an internal structure that fits insights as well as today,” Professor Stanley said.
This finding provides a compelling alternative theory for common assumptions that affect obliterating evidence of magnetic field elimination across rocky planets in the Northern Hemisphere.
____
C. Yang et al. 2025. Mars hemispherical magnetic field from a full sphere dynamo. Geophysical Research Book 52(3): E2024GL113926; doi: 10.1029/2024GL113926
Nintendo may announce its next console this week, a successor to the Nintendo Switch, which was released in March 2017 and sold 150 million units. There’s just one problem. That said, we already know almost everything about it. There is little that Nintendo can announce at this point that will come as a surprise to anyone who has been following the rumors closely.
Nintendo Switch 2 leaks started trickling in last summer and escalated to a flood this month. Last week, CES Technology Trade Show In Las Vegas, accessory maker Genki arrived with a complete model of Nintendo’s next console, which they were happy to show off behind closed doors to explain their upcoming product. You can also see detailed renderings on Genki’s website. It’s a slightly larger and more powerful version of the Switch console we know and love, with controllers that attach magnetically to the side of the screen rather than sliding in and out. Play while docked to your TV or on the go.
This is a very un-Nintendo approach. Aside from the NES/SNES, all of Nintendo’s consoles ushered in a revolution in form factors. There was the N64, with its pioneering analog sticks and three-pronged controller. GameCube looks like a stubby toy. Wii, motion control remote control included. Its successor, the Wii U, added a screen in the center of the controller. With the exception of the dual-screen DS and its successor, the 3DS, which added stereoscopic 3D to the console’s capabilities, this is the first time Nintendo has produced two consecutive consoles that look and act the same. They even share a name and logo. The most reliable information currently indicates that it will be called Nintendo Switch 2.
I won’t repeat any more details that were leaked about the Switch 2. They are easy to search and within the next day or so you can clearly see what is true and what is false. Nintendo has confirmed that the Switch 2 will share its back catalog with the Switch. This will allow all players to enjoy all the games they have purchased over the past eight years on their new console. We also know it won’t be out until April (June is my money), as it’s scheduled to come out in Nintendo’s next fiscal year. However, this is an unusual situation. We know almost everything about the console from gaming’s most secretive company even before it’s officially announced. How did it happen?
It was difficult to get a PS5 on release day. Photo: Charlie Tribalew/AFP/Getty Images
When the PlayStation 5 was released in 2020, the biggest talking point at the time was that people wouldn’t be able to get their hands on the PlayStation 5. Some customers who pre-ordered the PS5 received a package containing a bag of rice instead, but it was swapped with a vendor who was having trouble with the delivery chain. On eBay and other resale platforms, consoles were selling for two to three times the retail price. The supply-demand gap has dogged gaming consoles for at least the first two years, caused in part by manufacturing challenges during the pandemic. Nintendo probably wanted to avoid a similar situation.
We know that Nintendo’s manufacturing partners have been manufacturing parts for this console for a long time, over a year. The company aims to maintain large amounts of inventory in preparation for product launches. This is one of the reasons why so much information was leaked in advance. Various companies are already involved in the production of the Switch 2, and units and some units have been out for quite some time.
Nintendo also hasn’t gone after leakers or legally shut anything down in the way you might expect. The company’s only response to this deluge of unauthorized information, given to Japan’s Sankei Shimbun last week, was that “these images and videos are not official.” This suggests that Nintendo itself thought this might be inevitable. The company is delaying the announcement of its next console for as long as possible to preserve the survival of the phenomenally successful Switch, and said it doesn’t think these leaks will significantly damage its sales outlook.
The Switch 2 announcement will likely contain some surprises. What’s surprising is the rather un-Nintendo nature of this iterative console, and the piecemeal nature of what we’re discovering about it. Stay tuned for official announcements coming soon for more details.
what to play
Literally mow the grass. It’s literally just mowing the grass. Photo: Protostar
Effortless dad games for those who don’t want to spend time in the garden for a quiet January: It’s literally just mowing the grass. That’s exactly right. With a swipe, the small riding lawn mower eases its way through the ever-widening swathes of rough grass in your neighbor’s yard until the entire street is tidy. Cut the grass, collect hats, tap and admire different types of butterflies. It was my friend Patrick Klepek from the pro-gamer newsletter who brought this to my attention. cross play (We do a podcast together about navigating games with kids), and I was surprised to find myself playing it for a full 30 minutes straight. Am I getting old?
Available: iOS/Android
Estimated play time: 5 minutes or 1 hour, as long as you like
what to read
Dreams on a Pillow took 10 years to create. Photo: Rasheed Abueide
Games about Dreams on a Pillow 1948 Nakba Palestinian developer Rasheed Abueideh has reached his fundraising goal. I spoke to Abueide about the many obstacles he faced in trying to tell the Palestinian story through video games, challenges that no one should have to face.
Square Enix announces new policy The purpose is to protect staff from: Harassment by toxic fansit goes beyond restricting games and services for players who abuse support staff and developers.
Latest Great game in no timespeed running event Last weekend, we raised more than $2.5 million for charity. A personal highlight was the Crazy Taxi player accompanied by a live pop-punk band.
Messier 77 is a relatively nearby and well-known bright spiral galaxy with a supermassive black hole at its center.
Messier 77 concept by artist. It is characterized by its powerful black hole and accretion disk, as well as the polarized light of water masers located outside the Milky Way. Image credit: NSF / AUI / NRAO / S. Dagnello.
Messier 77 is a barred spiral galaxy located 62 million light-years away in the constellation Cetus.
Also known as NGC 1068, LEDA 10266, and Cetus A, it has an apparent magnitude of 9.6.
Messier 77 was discovered in 1780 by French astronomer Pierre Méchain, who initially identified it as a nebula. Méchain then relayed this discovery to his colleague, the French astronomer Charles Messier.
Messier believed that the extremely bright objects he saw were clusters of stars, but as technology advanced, their true status as a galaxy was recognized.
At 100,000 light-years in diameter, Messier 77 is one of the largest galaxies in the Messier catalog, and its gravity is enough to twist and distort other galaxies nearby.
It is also one of the closest galaxies to active galactic nuclei (AGNs).
These active galaxies are among the brightest objects in the universe, emitting light in many if not all wavelengths, from gamma rays and X-rays to microwaves and radio waves.
But Messier 77's accretion disk is hidden by a thick cloud of dust and gas, despite being a popular target for astronomers.
Several light-years in diameter, the outer accretion disk is dotted with hundreds of different water maser sources that have been hinting at deeper structures for decades.
Masers are clear beacons of electromagnetic radiation that shine at microwave or radio wavelengths. In radio astronomy, water masers, observed at a frequency of 22 GHz, are particularly useful because they can shine through many of the dusts and gases that block the wavelengths of light.
Bucknell University astronomer Jack Gallimore and his colleagues began observing Messier 77 with two goals in mind: astronomical mapping of the galaxy's radio continuum and measuring the polarization of water masers.
“Messier 77 is a bit of a VIP among active galaxies,” says Dr. CM Violette Impellizzeri, an astronomer at the Leiden Observatory.
“There's an accretion disk right next to the black hole, and it's unusually powerful. And because it's so close, it's been studied in great detail.”
But the study authors looked at Messier 77 in an entirely new way.
Their observations were recently upgraded High sensitivity array (HSA) consists of the Karl G. Jansky Very Large Array, the Very Long Baseline Array, and NSF's NRAO telescope at the Green Bank Telescope.
By measuring the water maser's polarization and the continuous radio emission from Messier 77, they reveal the compact radio source, now known as NGC 1068*, and the mysterious extended structure of the fainter emission. I created a map to
Mapping the astronomical distribution of galaxies and their water masers reveals that they are spread along structural filaments.
“These new observations reveal that the maser spot filaments are actually arranged like beads on a string,” Dr. Gallimore said.
“We were stunned to see that there was an apparent offset, or displacement angle, between the radio continuum, which describes the structure of the galaxy's core, and the position of the maser itself.”
“The configuration is unstable, so we're probably looking at a magnetically ejected source.”
Measuring the polarization of these water masers with HSA revealed significant evidence of a magnetic field.
“No one has ever seen polarization in water masers outside of our galaxy,” Dr. Gallimore said.
“Similar to the loop structures seen as prominences on the Sun's surface, the polarization patterns of these water masers clearly indicate that there is also a magnetic field at the root of these light-year-scale structures.”
“Looking at the filaments and making sure the polarization vector is perpendicular to the filaments is key to confirming that they are magnetically driven structures. It's exactly what you expected. It’s a thing.”
Previous studies of the region have suggested patterns, usually related to magnetic fields, but such conclusions were until recently beyond the scope of observational techniques.
The discovery reveals evidence for a compact central radio source (the galaxy's supermassive black hole), distinct polarization of water masers indicating structure within Messier 77's magnetic field, and spectacular extended signatures across the radio frequency continuum. It became.
Taken together, these findings indicate that magnetic fields are the underlying driving force for these phenomena.
However, many mysteries remain. For example, within the radio continuum map there is a diffuse, faint protrusion that the team has dubbed the foxtail foxtail, extending northward from the central region.
“When we set out on this, we said to ourselves, 'Let's really push the limits and see if we can get good continuum and polarization data,' and those goals were both It was a success,” Dr. Gallimore said.
“Using the NSF NRAO High Sensitivity Array, we detected the polarization of a water megamaser for the first time. We also created a very surprising continuum map, which we are still trying to understand.”
a paper The results will be explained today. Astrophysics Journal Letter.
_____
Jack F. Gallimore others. 2024. Discovery of polarized water vapor megamaser emission in molecular accretion disks. APJL 975, L9; doi: 10.3847/2041-8213/ad864f
Giant reed warbler migrating between Europe and Africa
AGAMI Photo Agency / Alamy Stock
Many migratory birds use the Earth's magnetic field as a compass, and others can use information from that field to more or less determine where they are on their mental map.
Greater Reed Warbler (Acrocephalus skillupaceus) appears to calculate geographic location by drawing data from various distances and angles between the magnetic field and the shape of the Earth. The study suggests that birds use magnetic information as a kind of “GPS,” telling them not only where to go, but also their initial whereabouts, they said. richard holland At Bangor University, UK.
“When we travel, we have a map that shows us where we are and a compass that shows us which direction to go to reach our destination,” he says. “We don't expect birds to have this much precision or knowledge about the entire planet. Yet, when they travel along their normal path, or even when they travel far from that path, they , and observe how the magnetic cues change.”
Scientists have known for decades that migratory birds rely on cues from the ocean. solar, star and earth's magnetic field To decide which direction to go. But using a compass to figure out direction and knowing where a bird is in the world are markedly different, and scientists are wondering if and how birds figure out their current map location. I'm still debating whether to do it or not.
Florian Packmore Germany's Lower Saxony Wadden Sea National Park Administration suspected that birds could detect detailed aspects of magnetic fields to determine their global location. Specifically, magnetic obliquity (the change in the angle of the Earth's surface relative to magnetic field lines) and magnetic declination (the difference in orientation between the geographic and magnetic poles) are used to better understand where you are in the world. He thought he might be able to do it.
To test their theory, Packmore, Holland and colleagues captured 21 adult reed warblers in Illmitz, Austria, on their migration route from Europe to Africa. So the researchers temporarily placed the birds in an outdoor aviary, where they used a Helmholtz coil to disrupt the magnetic field. They artificially altered the inclination and declination in a way that corresponded to the location of Neftekamsk, Russia, 2,600 kilometers away. “That's way off course for them,” Packmore says.
The researchers then placed the birds in special cages to study their migratory instincts and asked two independent researchers, who were unaware of changes in the magnetic field, to record which direction the birds headed. In the changed magnetic field conditions, most birds showed a clear tendency to fly west-southwest, as if trying to return to their migratory route from Russia. In contrast, when the magnetic field was unchanged, the same birds attempted to fly south-southeast from Austria.
This suggests that the birds believed they were no longer in Austria, but Russia, based solely on magnetic inclination and declination, Packmore said.
“Of course they don't know it's Russia, but it's too far north and east from where they should be,” Holland says. “And at that point, they look at their compass system and figure out how to fly south and west.”
However, the neurological mechanisms that allow birds to sense these aspects of the Earth's magnetic field are still not fully understood.
“This is an important step in understanding how the magnetic maps of songbirds, especially the great reed warbler, work,” he says. Nikita Chernetsov The professor at the Institute of Zoology of the Russian Academy of Sciences in St. Petersburg was not involved in the study.
The study confirms that the great reed warbler relies on these magnetic fields for positioning, but that doesn't mean all birds do, he added. “Not all birds work the same.”
Packmore and Holland said the birds were released two to three weeks after the study, at which point they were able to continue their normal migration. In fact, one of the birds they studied was captured a second time a year later. This means that the researchers' work did not interfere with the birds' successful migration.
This groundbreaking achievement will improve our understanding of the Sun’s atmosphere and shed light on how its changing conditions affect our technology-dependent society.
The Inouye Solar Telescope has released the first map of the magnetic field signal in the solar corona measured using the Zeeman effect. Image courtesy of NSF/NSO/AURA/NASA’s Solar Dynamics Observatory.
The Earth’s magnetic field protects us from the solar wind, protects our atmosphere and makes life possible.
But electromagnetic fields and high-energy particles from extreme solar activity could disrupt satellites, power grids, and other systems necessary for an increasingly technological society.
Understanding these dynamic interactions, which change on timescales ranging from days to centuries, is crucial to safeguarding our infrastructure and current ways of life.
Measuring the magnetic properties of the Sun’s corona, or outer atmosphere, has long challenged astronomers and the limits of technology.
today, Daniel K. Inouye Solar TelescopeLocated near the summit of Haleakala on the Hawaiian island of Maui, the facility is a state-of-the-art facility designed to study coronas.
The satellite has produced the first and most detailed map of the coronal magnetic field to date, taking an important first step in solving these mysteries.
“Inoue’s achievements in mapping the Sun’s coronal magnetic field are a testament to the innovative design and capabilities of this pioneering and unique observatory,” said Dr. Tom Shad, NSF National Solar Observatory investigator.
“This groundbreaking discovery is expected to greatly improve our understanding of the Sun’s atmosphere and its impact on the solar system.”
The researchers used the Zeeman effect, which measures magnetic properties by observing the splitting of spectral lines, to create a detailed map of the magnetic field of the solar corona.
“Spectral lines are distinct lines that appear at particular wavelengths in the electromagnetic spectrum and represent light absorbed or emitted by atoms and molecules,” they explained.
“These lines are unique to each atom and molecule and act like a fingerprint. By looking at the spectrum, scientists can determine the chemical composition and physical properties of an object.”
“When exposed to a magnetic field like the Sun’s, these lines split apart, giving us insight into the magnetic properties of the object.”
Previous attempts to detect such signals, last reported 20 years ago, have lacked the detail and regularity needed for widespread scientific investigation.
Now, Inouye’s unparalleled capabilities make it possible to study these important signals in detail and on a regular basis.
The solar corona can usually only be seen during a total solar eclipse, when most of the Sun’s light is blocked and Earth’s sky becomes dark.
But the Inouye Telescope uses a technique called coronagraphy to create an artificial eclipse that allows it to detect extremely faint polarized signals, highlighting its unparalleled sensitivity and cementing its status as a unique window into viewing our home star.
This telescope is Cryogenic near-infrared spectropolarimeter (Cryo-NIRSP) is one of the telescope’s main instruments used to study the corona and map its magnetic field.
“Just as detailed maps of the Earth’s surface and atmosphere have improved the accuracy of weather forecasts, this remarkably complete map of the magnetic field of the Sun’s corona will help us more accurately predict solar storms and space weather,” said Dr. Carrie Black, program director for NSF’s National Solar Observatory.
“The invisible yet incredibly powerful forces captured in this map will continue to drive solar physics for the next century and beyond.”
“Mapping the strength of the corona’s magnetic field is a fundamental scientific advance not only for solar research but for astronomy in general,” said Dr. Christoph Keller, director of the National Solar Observatory.
“This marks the beginning of a new era in understanding how stars’ magnetic fields affect planets in our solar system and the thousands of exoplanetary systems currently known.”
_____
This article has been edited from an original release by the National Solar Observatory.
A jellyfish-shaped robot made from magnetic fluid can be controlled with light through an underwater obstacle course, and swarms of these soft robots could be useful for delivering chemicals throughout liquid mixtures or moving fluids through a lab-on-a-chip.
Ferrofluid droplets are made of magnetic nanoparticles suspended in oil, and can move across a flat surface and change shape when guided in different directions by a magnet. When these droplets are immersed in water and exposed to light, Sun Meng Meng, a researcher from the Max Planck Institute for Intelligent Systems in Germany, and his colleagues have succeeded in creating an object that defies gravity.
When ferrofluid absorbs light (and it’s particularly good at that, because it’s black), it heats up, causing tiny bubbles inside it to expand. This makes the droplets below the surface lighter and more buoyant, allowing them to float upwards, Sun says.
He and his colleagues built a soft robot with droplets of magnetic fluid encased in a jellyfish-shaped hydrogel shell, and then tested it. The researchers devised an obstacle course at the bottom of a tank of water that included a variety of platforms of different heights. They guided the robot through the course and had it navigate over the platforms.
In one experiment, they lined up three robotic jellyfish on the bottom of a tank and heated them with a laser, causing them to move upward one after the other. Sunlight focused by a magnifying glass had a similar effect, causing the jellyfish to float vertically.
Hamid Marvi, the Arizona State University researcher, says controlling an entire swarm of droplets simultaneously could one day be useful for delivering medicines or performing other functions in the human body. By encasing them in hydrogel, he says, light could be used to guide the ferrofluid droplets and move the hydrogel itself, enabling complex movements.
But Mulvey says many details need to be worked out before the ferrofluid can be used for medical purposes, such as whether it’s safe to ingest it. Sun and his colleagues hope to answer some of those open questions. For example, they hope to find a way to use optical fibers that can be inserted into the body to guide the robot, rather than lasers or sunlight.
American theoretical physicist Joseph Polczynski once said that the existence of magnetic monopoles is “one of the safest bets you can make about physics that has yet to be seen.” In the search for these particles that have magnetic charges and are predicted by several theories that extend the standard model, Moedal (Monopole and Exotic Detectors at the LHC) Although the collaboration has yet to prove Polczynski correct, its latest discovery represents a major advance. The new results narrow the search window for these hypothetical particles.
Generation of monopole pairs by Schwinger mechanism. Image credit: MoEDAL Collaboration / CERN.
At CERN's Large Hadron Collider (LHC), interactions between protons or heavy ions can produce pairs of magnetic monopoles.
In collisions between protons, protons can be formed from a single virtual photon (Dorrell-Yang mechanism) or from the fusion of two virtual photons (photon fusion mechanism).
Through a process called the Schwinger mechanism, pairs of magnetic monopoles can also be generated from the vacuum of huge magnetic fields produced by near-miss collisions of heavy ions.
Since starting data acquisition in 2012, MoEDAL has achieved several firsts, including conducting the first search for magnetic monopoles produced by photon fusion and Schwinger mechanisms at the LHC. Ta.
inside First part of the latest researchMoEDAL physicists explored monopoles and highly charged objects (HECOs) produced via the Dorell-Yang mechanism and the photon fusion mechanism.
This search was based on proton-proton collision data collected during Experiment 2 at the LHC using the complete MoEDAL detector for the first time.
The complete detector consists of two main systems that sense magnetic monopoles, HECO, and other highly ionizing virtual particles.
First, magnetic monopole and HECO trajectories can be permanently registered without background signals from standard model particles. The second system consists of an approximately 1-ton capture volume designed to capture magnetic monopoles.
Although the researchers did not find any magnetic monopoles or HECOs in their latest scan of the trapping volume, the masses and production rates of these particles were determined for different values of particle spin, a unique form of angular momentum. limits have been set.
For magnetic monopoles, a mass limit of 1 to 10 times the Dirac charge (gD), the basic unit of magnetic charge, is set, excluding the existence of monopoles with masses as high as about 3.9 trillion electron volts (TeV). I did. .
For HECO, a mass limit was established for charges from 5e to 350e, where e is the electronic charge, and the presence of HECO with masses in the range up to 3.4 TeV was excluded.
“MoEDAL's search reach for both monopoles and HECOs allows the collaboration to explore vast swaths of the theoretical 'discovery space' for these hypothetical particles,” said a spokesperson for the MoEDAL collaboration. said Dr. James Pinfold.
in their second studyMoEDAL scientists focused on searching for monopoles produced via the Schwinger mechanism in heavy ion collision data collected during LHC Experiment 1.
In a unique effort, we scanned a decommissioned section of the CMS experimental beam pipe for trapped monopoles instead of the trapping volume of the MoEDAL detector.
Again, the team found no monopoles, but set the strongest mass constraints yet for Schwinger monopoles with charges between 2 gD and 45 gD, ruling out the existence of monopoles with masses up to 80 GeV. did.
“A crucial aspect of the Schwinger mechanism is that the production of complex monopoles is not suppressed compared to the production of elementary monopoles, as is the case with Dorell-Yang and photon fusion processes,” Pinfold said. Ta.
“Therefore, if monopoles are composite particles, this and the previous Schwinger monopole search may have been the first ever chance to observe monopoles.”
_____
Moedal collaboration. 2024. Searching for highly ionized particles in pp collisions in LHC Run-2 using the Full MoEDAL detector. arXiv: 2311.06509
B. Acharya other. 2024. MoEDAL explores magnetic monopoles generated by the Schwinger effect in CMS beam pipes. arXiv: 2402.15682
Recovering ancient records of the Earth's magnetic field is difficult because the magnetization of rocks is often reset by heating during burial due to tectonic movements over a long and complex geological history. Geoscientists from MIT and elsewhere have shown that rocks in West Greenland's Isua supercrustal zone have experienced three thermal events throughout their geological history. The first event was the most important, heating rocks to 550 degrees Celsius about 3.7 billion years ago. His two subsequent phenomena did not heat the region's northernmost rocks above 380 degrees Celsius. The authors use multiple lines of evidence to test this claim, including paleomagnetic field tests, metamorphic mineral assemblages across the region, and temperatures at which the radiometric ages of observed mineral assemblages are reset. They use this body of evidence to argue that an ancient record of Earth's magnetic field from 3.7 billion years ago may be preserved in the striated iron layer at the northernmost edge of the magnetic field. .
Earth's magnetic field lines. Image credit: NASA's Goddard Space Flight Center.
In a new study, Professor Claire Nicholls from the University of Oxford and colleagues examined a range of ancient iron-bearing rocks from Isua, Greenland.
Once locked in place during the crystallization process, iron particles effectively act as tiny magnets that can record both the strength and direction of a magnetic field.
Researchers found that 3.7 billion-year-old rocks exhibited magnetic field strengths of at least 15 microteslas, comparable to modern magnetic fields (30 microteslas).
These results provide the oldest estimates of the strength of Earth's magnetic field derived from whole rock samples, providing a more accurate and reliable estimate than previous studies using individual crystals.
“It's very difficult to extract reliable records from rocks this old, so it was really exciting to see the primary magnetic signals start to emerge when we analyzed these samples in the lab,” Professor Nichols said. said.
“This is a very important step forward in our efforts to understand the role of ancient magnetic fields in the creation of life on Earth.”
Although the strength of the magnetic field appears to remain relatively constant, the solar wind is known to have been significantly stronger in the past.
This suggests that surface protection from the solar wind may have strengthened over time, thereby allowing life to leave the protection of the oceans and migrate to the continents.
The Earth's magnetic field is created by the mixing of molten iron within a fluid outer core, driven by buoyancy as the inner core solidifies, forming a dynamo.
During the early stages of Earth's formation, a solid inner core had not yet formed, leaving unanswered questions about how the initial magnetic field was maintained.
These new results suggest that the mechanisms driving Earth's early dynamo were as efficient as the solidification processes that generate Earth's magnetic field today.
Understanding how the strength of Earth's magnetic field has changed over time is also key to determining when Earth's interior solid core began to form.
This helps us understand how fast heat is escaping from the Earth's deep interior, which is key to understanding processes such as plate tectonics.
A key challenge in reconstructing Earth's magnetic field back in time is that any event that heats rocks can change the preserved signal.
Rocks in the Earth's crust often have long and complex geological histories that erase information about previous magnetic fields.
However, the Isua supercrustal zone has a unique geology, sitting on a thick continental crust and protected from extensive tectonic movements and deformation.
This allowed scientists to build clear evidence for the existence of magnetic fields 3.7 billion years ago.
The results may also provide new insights into the role of magnetic fields in shaping the development of Earth's atmosphere as we know it, particularly regarding the release of gases into the atmosphere.
“In the future, we hope to expand our knowledge of Earth's magnetic field before oxygen increased in the Earth's atmosphere about 2.5 billion years ago by examining other ancient rock sequences in Canada, Australia, and South Africa. “We believe that this is the case,” the authors said.
“A better understanding of the strength and variability of ancient Earth's magnetic field will help determine whether the planet's magnetic field was important for harboring life on the planet's surface and its role in the evolution of the atmosphere. Masu.”
of study Published in Geophysical Research Journal.
_____
Claire IO Nichols other. 2024. Possible Archean record of geomagnetism preserved in the Isua supercrustal zone of southwestern Greenland. Geophysical Research Journal 129 (4): e2023JB027706; doi: 10.1029/2023JB027706
New and impressive images of the supermassive black hole located at the center of our galaxy show that its powerful magnetic field twists and rotates in a spiral pattern.
This is a never-before-seen view of Sagittarius A* (or Sgr A*), the massive black hole in the Milky Way galaxy that consumes nearby light and matter.
The images suggest similarities in structure between this black hole and the black hole in the galaxy M87. Although the black hole in M87, which was imaged for the first time, is over 1,000 times larger than Sagittarius A*, both exhibit strong, organized magnetic fields.
This pattern hints that many, if not all, black holes may share common traits, according to the scientists who published their findings in the Astrophysics Journal Letter on Wednesday.
“We’ve discovered that strong, orderly magnetic fields are crucial in how black holes interact with surrounding gas and matter,” said study co-leader and NASA Hubble Fellowship Program co-author, Einstein Fellow Sarah Isaun, as stated in a press release.
Isaun worked with an international team of astronomers known as the Event Horizon Telescope to conduct the research. This team comprises over 300 scientists from 80 institutions worldwide.
This same collaboration captured the first direct visual evidence of Sagittarius A* in 2022 and also studied the M87 galaxy, which is located approximately 53 million light-years away from Earth.
The magnetic field around the massive black hole at the center of the M87 galaxy, known as M87*, is believed to play a vital role in its extraordinary behavior. Black holes emit powerful jets of electrons and other subatomic particles into space at nearly the speed of light.
Although no such bursts of activity have been observed from Sagittarius A*, the similarities between the two black holes suggest that hidden jets may still be detected. Researchers suggest this possibility in the new images.
According to astronomers’ best models of black hole evolution, the magnetic field within the accretion disk must be strong enough to push the accreted plasma out into the surroundings. New results from Sagittarius A*, the 4.3 million solar mass black hole at the center of the Milky Way galaxy, and its much larger cousin M87* provide the first direct observational evidence supporting these models.
This image from the Event Horizon Telescope shows a polarized view of Sagittarius A*. The lines superimposed on this image show the direction of polarization associated with the magnetic field around the black hole’s shadow. Image credit: EHT Collaboration.
In 2022, EHT collaboration The first image of Sagittarius A*, about 27,000 light-years from Earth, has been released, showing that the Milky Way’s supermassive black hole looks very good despite being more than 1/1000th smaller and lighter in mass than M87. revealed that they are similar.
This led scientists to wonder if the two men had more in common than just their looks. To find out, they decided to study Sagittarius A* in polarized light.
Previous studies of the light surrounding M87* revealed that the magnetic field around the supermassive black hole causes powerful jets of matter to be ejected into the surrounding environment.
Based on this study, new EHT images reveal that the same may be true for Sagittarius A*.
“What we’re seeing now is a strong, twisted, organized magnetic field near the black hole at the center of the Milky Way,” said astronomers at the Harvard University & Smithsonian Center for Astrophysics. said Dr. Sarah Isaun.
“In addition to having a polarization structure that is strikingly similar to that seen in the much larger and more powerful M87* black hole, Sagittarius A* has a polarization structure that is strikingly similar to that seen in the much larger and more powerful M87* black hole. We found that strong, well-ordered magnetic fields are important for how they act.”
Light is a vibrating or moving electromagnetic wave that allows us to see objects. Light can oscillate in a particular direction, which scientists call polarization.
Polarized light is all around us, but to the human eye it is indistinguishable from “normal” light.
In the plasma around these black holes, particles swirling around magnetic field lines impart a polarization pattern perpendicular to the magnetic field.
This will allow astronomers to see in clearer detail what’s happening in the black hole region and map its magnetic field lines.
“By imaging polarized light from glowing gas near a black hole, we are directly inferring the structure and strength of the magnetic field that flows through the streams of gas and matter that the black hole feeds and ejects.” said Dr. Angelo Ricarte. Astronomer at Harvard University and the Harvard & Smithsonian Center for Astrophysics.
“Polarized light can tell us much more about astrophysics, the properties of the gas, and the mechanisms that occur when black holes feed.”
But imaging black holes under polarized light isn’t as easy as wearing polarized sunglasses. This is especially true for Sagittarius A*. Sagittarius A* changes so quickly that you can’t stand still and take a photo.
Imaging supermassive black holes requires sophisticated tools beyond those previously used to capture a more stable target, M87*.
“Sagittarius A*s are like enthusiastic toddlers,” said Avery Broderick, a professor at the University of Waterloo.
“For the first time, we see invisible structures that guide matter within a black hole’s disk, drive plasma to the event horizon, and help the plasma grow.”
“Sagittarius A* moves around while trying to photograph it, so it was difficult to even construct an unpolarized image,” said astronomer Dr. Jeffrey Bower of the Institute of Astronomy and Astrophysics, Academia Sinica in Taipei. Told.
“The first image is an average of multiple images from the movement of Sagittarius A*.”
“I was relieved that polarized imaging was also possible. Some models had too much scrambling and turbulence to build polarized images, but nature isn’t that cruel. did.”
Professor Maria Felicia de Laurentiis, University of Naples Federico II, said: “Using samples of two black holes with very different masses and host galaxies, we can determine what they agree on and what they do not agree on.” It’s important.
“Since both point us toward strong magnetic fields, this suggests that this may be a universal and perhaps fundamental feature of this type of system.”
“One similarity between these two black holes could be a jet. But while we imaged a very obvious black hole in M87*, we have yet to find one in Sagittarius A*. not.”
Collaboration with Event Horizon Telescope. 2024. Horizon telescope results for the first Sagittarius A* event. VII. Polarization of the ring. APJL 964, L25; doi: 10.3847/2041-8213/ad2df0
Collaboration with Event Horizon Telescope. 2024. Horizon telescope results for the first Sagittarius A* event. VIII. Physical interpretation of polarization rings. APJL 964, L26; doi: 10.3847/2041-8213/ad2df1
This is a supermassive black hole at the center of a galaxy that we have never seen before. The image reveals a swirling magnetic field around Sagittarius A* (Sgr A*), suggesting it may be producing jets of high-energy material that astronomers have not yet seen.
This photo was taken by a network of observatories around the world operating as a single giant telescope called the Event Horizon Telescope (EHT). In 2022, the first images of Sgr A* were produced, revealing light emanating from swirling hot plasma set against the dark background of a black hole's event horizon. There, light cannot escape the extreme gravity.
Now, EHT researchers Jiri Yunshi The researchers from University College London measured how this light is polarized, or the direction of the electromagnetic field, and showed the direction and strength of the magnetic field around Sgr A*.
This image is very similar to the magnetic field of M87*, the first black hole studied by EHT. Given that M87* is about 1,500 times more massive than Sgr A*, this suggests that supermassive black holes may have similar structures regardless of their size, Yunshi says.
The two black holes photographed by the Event Horizon Telescope are strikingly similar.
European Southern Observatory (ESO)
One major difference between M87* and the black holes in our galaxy is the absence of visible high-energy jets visible from Sgr A*. This lack has long puzzled astronomers, but the fact that Sgr A* has a magnetic field like M87* suggests that our galaxy's black hole may also have jets. It suggests.
“There are very interesting hints that there may be additional structures,” Yunshi says. “I think something very exciting could be happening at the center of the galaxy, and we need to track these results.”
This makes sense given other evidence for jets that may have existed long before the galaxy's history, such as Fermi bubbles, large balls of X-ray-producing plasma above and below the Milky Way. Masu.
In addition to revealing potential hidden jets, the properties of magnetic fields also solve other astrophysical mysteries, such as how particles like cosmic rays and neutrinos are accelerated to ultrahigh energies. This could help solve the problem, Yunshi said. “Magnetic fields are the basis of all of this. Anything that yields further insight into how black holes and magnetic fields interact is of just fundamental importance to astrophysics.”
Yunshi and his colleagues hope to use a larger telescope network and more advanced equipment to take more images of Sgr A*, which will help them understand the nature of the magnetic field and how it directs the jet. This will deepen your understanding of what is being generated. EHT plans to begin these observations in April, but processing the data could take several years.
New technology allows water droplets to be guided precisely around obstacle courses to trigger chemical reactions
Jonathan Knowles/Getty Images
By placing tiny magnetic particles inside ordinary water droplets, you can turn them into liquid acrobats. Droplets can climb steps, jump over obstacles, and initiate chemical reactions. This level of control could be useful for drug delivery and the creation of more complex lab-on-a-chip technologies.
Fan Shilin He and his colleagues at Sun Yat-sen University in China created a surface with tiny grooves and covered it with a superhydrophobic, or wet-resistant, varnish. They know that a water droplet resting on such a groove can spontaneously jump up due to the pressure difference between the bottom of the droplet, which is deformed by the small groove, and the rounded and less constrained top part. I did.
The researchers wanted to create this pressure difference on demand. They added small magnetic particles to each droplet and placed an electromagnet beneath the groove. When the electromagnet was turned on, some of the particles, or droplets, were drawn into the groove. When I turned it off, the water droplet shape bounced and flew upwards as if from a slingshot.
Using this technique, the team was able to enable droplets to hop down millimeter-scale stairs and overcome small obstacles. The researchers were also able to direct a droplet into the narrow space between two wires and connect a circuit to light a light bulb.
Xiao Yan Researchers from China’s Chongqing University say this is a creative way to control pressure-based droplet jumps and could become a valuable tool for precisely transporting chemical droplets. It has said.
In one experiment, researchers plunged and mixed droplets into a liquid chemical sample under a microscope lens, allowing them to observe the resulting chemical reaction from start to finish. Another experiment involved mixing two droplets with a third in a closed box, which would have been ruined if the researchers had had to open the box to let air in. The reaction was initiated remotely.
Such precise chemical control can be applied to drug delivery. Huang hopes the technology will also advance “lab-on-a-chip” technology, an effort to miniaturize complex biochemical experiments that typically require a lot of space and glassware. He proposes a “lab-on-stacked chip” in which droplets jump vertically between levels to generate many reactions in parallel.
This website uses cookies so that we can provide you with the best user experience possible. Cookie information is stored in your browser and performs functions such as recognising you when you return to our website and helping our team to understand which sections of the website you find most interesting and useful.
Strictly Necessary Cookies
Strictly Necessary Cookie should be enabled at all times so that we can save your preferences for cookie settings.
