SPACE/COSMOS
Listening to Sun's 'heart' hints our star could be changing
image:
A split image showing an active Sun during solar maximum (on the left, taken in 2014) and a quiet Sun during solar minimum (on the right, taken in 2019).
view moreCredit: NASA/SDO
The Sun's internal 'biorhythm' – which plays a critical role in the space weather we experience on Earth – has mysteriously changed over the past 40 years, a new study suggests.
Listening to tiny sound waves inside our star's 'heart' led researchers to discover that it may be entering "a different mode of behaviour". They now need to explore what this means.
The research, published today in Monthly Notices of the Royal Astronomical Society, is of particular significance to space weather.
Solar activity rises and falls in 11‑year cycles, producing solar flares, and ejections of highly charged particles and coronal mass ejections that give rise to geomagnetic storms and aurorae.
This activity, and its cyclic variation, has its origins in the Sun's interior, in processes that regenerate and reorganise the Sun's magnetic field.
Understanding what drives the solar cycle is therefore crucial for making predictions of space weather, which can disrupt satellites, communications, GPS systems and power grids on Earth.
Traditional measures of solar activity track these emissions and other surface phenomena like sunspots, but they do not look under the solar surface. However, by 'listening' to tiny sound waves inside the Sun – a technique known as helioseismology – it is possible to do just that. By tracking changes in the otherwise hidden solar interior, the team found a different picture emerged of the Sun's activity over the past few cycles to the one given by the traditional measures.
Using almost 40 years of helioseismic data from six telescopes around the world in the Birmingham Solar Oscillations Network (BiSON), the international team of researchers uncovered a gradual change in structure just beneath the surface that has spanned multiple cycles, with the current solar cycle 25 showing particularly strong signatures of these changes.
They discovered that solar magnetic activity is being squeezed into an increasingly shallow layer just below the visible surface, signposting long-term changes to the Sun's active behaviour.
Lead author Professor Bill Chaplin, from the University of Birmingham, said: "The Sun has its own 'active biorhythm' creating rising and falling magnetic activity that shapes space weather. However, traditional surface measures don't capture the full story – that the Sun may be entering a different mode of behaviour unfolding over decades.
"We have uncovered evidence of systematic changes in the solar activity cycle. Crucially, magnetic activity is becoming more tightly confined near the surface with each cycle. This is the first such discovery and would have been impossible without the long BiSON observations."
The researchers analysed the p-mode oscillations – formed by global sound waves inside the Sun – whose frequencies shift in response to solar magnetic activity. This allowed them to determine how the Sun's internal structure changed across solar cycles 22–25, from 1987 to 2025.
They grouped oscillations into low-, mid-, and high-frequency bands to probe different depths beneath the solar surface. The team then compared these frequency shifts with traditional measures of solar activity to reach three main conclusions:
- Evidence of changing behaviour – the link between oscillation frequencies and traditional activity measures has shifted significantly since Cycle 23, indicating long-term evolution in the Sun's internal processes.
- Surface confinement of structural changes – the combined behaviour of low-, mid-, and high-frequency modes shows that solar-cycle-driven structural changes are becoming increasingly confined to shallow layers, within 1,000km of the Sun's surface.
- Reinterpreting the strength of the latest cycle – Cycle 25 appears weaker in traditional surface indicators but comparably strong when seen in the high-frequency helioseismic data.
Professor Sarbani Basu, from Yale University, said: "We discovered that the relationship between internal solar oscillations and surface activity has evolved over the past few cycles.
"This trend cannot be explained simply by weaker magnetic fields. Instead, it indicates a structural reorganisation of how the Sun's magnetic activity is stored beneath the surface."
Ongoing collection and analysis of BiSON solar data over what remains of Cycle 25 and into the upcoming Cycle 26 will be crucial in determining whether the changes discovered in the Sun's activity point to a sustained, systematic change in solar magnetic behaviour.
ENDS
Images & captions
Caption: As the Sun's activity varies over each 11-year solar cycle – from periods of high activity (solar maxima) to low activity (solar minima) – so the Sun's oscillations, which are due to sound waves in the Sun's interior, increase and decrease in frequency. The oscillations therefore track and probe the Sun's active biorhythm.
Credit: W. J. Chaplin
Caption: A split image showing an active Sun during solar maximum (on the left, taken in 2014) and a quiet Sun during solar minimum (on the right, taken in 2019).
Credit: NASA/SDO
As the Sun's activity varies over each 11-year solar cycle – from periods of high activity (solar maxima) to low activity (solar minima) – so the Sun's oscillations, which are due to sound waves in the Sun's interior, increase and decrease in frequency. The oscillations therefore track and probe the Sun's active biorhythm.
Credit
W. J. Chaplin
Further information
The paper ‘Subsurface structural changes associated with successive 11-yr solar activity cycles have been progressively more confined near the surface: new helioseismic results on Cycles 22–25 from BiSON’ by Chaplin et al. has been published in Monthly Notices of the Royal Astronomical Society. DOI: 10.1093/mnras/stag847.
Notes for editors
About the Royal Astronomical Society
The Royal Astronomical Society (RAS), founded in 1820, encourages and promotes the study of astronomy, solar-system science, geophysics and closely related branches of science.
The RAS organises scientific meetings, publishes international research journals, recognises outstanding achievements by the award of medals and prizes, maintains an extensive library, supports education through grants and outreach activities and represents UK astronomy nationally and internationally. Its more than 4,000 members (Fellows), a third based overseas, include scientific researchers in universities, observatories and laboratories as well as historians of astronomy and others.
The RAS accepts papers for its journals based on the principle of successful peer review, following which experts on the Editorial Boards accept the papers for publication. The Society issues press releases based on a similar principle, but the organisations and scientists concerned have overall responsibility for their content.
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About the University of Birmingham
The University of Birmingham is ranked amongst the world's top 100 institutions. Its work brings people from across the world to Birmingham, including researchers, teachers and more than 40,000 students from over 150 countries.
England's first civic university, the University of Birmingham is proud to be rooted in of one of the most dynamic and diverse cities in the country. A member of the Russell Group and a founding member of the Universitas 21 global network of research universities, the University of Birmingham has been changing the way the world works for more than a century.
Journal
Monthly Notices of the Royal Astronomical Society
Article Title
‘Subsurface structural changes associated with successive 11-yr solar activity cycles have been progressively more confined near the surface: new helioseismic results on Cycles 22–25 from BiSON’
Article Publication Date
28-May-2026
Weighing newborn planets using their dusty fingerprints
Astronomers discover new method to estimate masses of planets using the dust in the protoplanetary disk
image:
Simulation of a planet embedded in a protoplanetary disc, causing disc material to pile up in a ring exterior to its orbit – Credit: Amena Faruqi / University of Warwick
view moreCredit: Amena Faruqi / University of Warwick
A team of astronomers, led by University of Warwick in collaboration with researchers at MIT and McMaster, have developed a novel method to use the properties of dust rings around stars to estimate the masses of newborn planets. Published in The Astrophysical Journal, this research offers astronomers a new way to find and characterise planets that are too deeply embedded in their birth environment to be seen directly.
Swirling disks of gas and dust surrounding young stars are the environments in which planets form. New powerful telescopes, such as ALMA, have revealed that many of these protoplanetary disks contain striking ring-shaped structures. These have long been suspected to be clues to the planets potentially orbiting within the disks, but until now robust methods to interpret them have proved elusive.
"These bright rings are not just beautiful structures - they are essentially planetary fingerprints," said lead author, Amena Faruqi, PhD student, Astronomy and Astrophysics Group, University of Warwick. "We’ve long understood that the rings could be created from concentrated dust that piles up just beyond the orbit of young, embedded planets, but we’ve been so far unable to link features of these rings to planet masses.
By reading ‘between the rings,’ we have now found a way to reconstruct the masses of the planets that create the rings, even when those planets are too faint or too embedded to observe directly.”
The research team used detailed computer simulations to determine how planets of different masses shape the dust rings around them. They discovered that a ring's width, the location of its brightest point, and the amount of dust it contains all carry tell-tale signatures of the planet responsible.
Crucially, the team identified a simple mathematical relationship between the location of a ring's brightness peak and the mass of its host planet, one that holds regardless of the observing wavelength or the size of the dust grains being imaged. This implies that astronomers can apply the method to existing observations without needing detailed knowledge of disk conditions.
To validate their approach, the researchers applied their method to PDS 70, one of the few systems where planets have been directly imaged inside their disk. They recovered a mass for the planet PDS 70c that is in strong agreement with independent estimates. They also applied the technique to five disks from the recent exoALMA survey, predicting new mass estimates for the planets potentially lurking within them.
Co-author Dr Jessica Speedie, 51 Pegasi b Postdoctoral Fellow, Massachusetts Institute of Technology (MIT) added: “One of the strengths of this work is that it doesn't stay in the realm of theory - we've been able to take these simulation results and apply them directly to real observed systems. Using the PDS 70 system as an observational laboratory in particular enabled a real verification of the approach, giving us confidence that these methods are genuinely ready to be applied widely as soon as possible. "
The findings open up new possibilities for disk observations that will help confirm the existence of planets suspected to be lurking in disks, reveal entirely new ones, and could shed light on processes which may have played a role in the formation of our own Solar System.
Senior co-author Professor Emeritus Ralph Pudritz, Department of Physics and Astronomy, McMaster University: “Another striking result of the simulations is that, in typical discs, more massive forming planets can trap as much as 20 times the mass of Earth of dust within these rings. This confirms ALMA observations – but raises the question of why new planets have not been detected in the trapped dust and pebbles of the ring. Our results suggest that the dust is sufficiently abundant and concentrated enough to potentially kick-off planet formation. This is an important insight that will initiate further observations and theory.”
Senior co-author Dr Farzana Meru, Reader, Department of Physics, University of Warwick concluded: "This work gives observers a new practical toolkit for connecting what we see in dust rings directly to the masses of the planets creating them. What excites me most is the timing. With ALMA delivering increasingly detailed disk images, and future facilities on the horizon, there has never been a better moment to develop these methods.
“Combining our dust-based diagnostics with gas pressure observations will open up a powerful new window onto the hidden planets shaping these disks and the diverse planetary systems they will go on to form."
ENDS
Notes to Editors
The paper "Reading between the Rings: Observed Dust Ring Properties as Probes of Planet Masses" is published in The Astrophysical Journal. DOI: 10.3847/1538-4357/ae6272
Simulation - Simulation of a planet embedded in a protoplanetary disc, causing disc material to pile up in a ring exterior to its orbit – Credit: Amena Faruqi / University of Warwick
GIF- Simulation images showing how tripling the planet mass changes the position of the dust ring. The ring position can be used to determine the mass of the planet causing it. – Credit: Amena Faruqi / University of Warwick
Image - Known as the Disk Substructures at High Angular Resolution Project (DSHARP), this “Large Program” of ALMA has yielded stunning, high-resolution images of 20 nearby protoplanetary disks and given astronomers new insights into the variety of features they contain and the speed with which planets can emerge. Credit: ALMA (ESO/NAOJ/NRAO), S. Andrews et al.; NRAO/AUI/NSF, S. Dagnello
For more information please contact:
Matt Higgs, PhD | Media & Communications Officer (Warwick Press Office)
Email: Matt.Higgs@warwick.ac.uk | Phone: +44(0)7880 175403
About the University of Warwick
Founded in 1965, the University of Warwick is a world-leading institution known for its commitment to era-defining innovation across research and education. A connected ecosystem of staff, students and alumni, the University fosters transformative learning, interdisciplinary collaboration, and bold industry partnerships across state-of-the-art facilities in the UK and global satellite hubs. Here, spirited thinkers push boundaries, experiment, and challenge convention to create a better world.
Simulation images showing how tripling the planet mass changes the position of the dust ring. The ring position can be used to determine the mass of the planet causing it. – Credit: Amena Faruqi / University of Warwick
Credit
Amena Faruqi / University of Warwick
Known as the Disk Substructures at High Angular Resolution Project (DSHARP), this “Large Program” of ALMA has yielded stunning, high-resolution images of 20 nearby protoplanetary disks and given astronomers new insights into the variety of features they contain and the speed with which planets can emerge. Credit: ALMA (ESO/NAOJ/NRAO), S. Andrews et al.; NRAO/AUI/NSF, S. Dagnello
Credit
ALMA (ESO/NAOJ/NRAO), S. Andrews et al.; NRAO/AUI/NSF, S. Dagnello
Journal
The Astrophysical Journal
Method of Research
Experimental study
Subject of Research
Not applicable
Article Title
Reading between the Rings: Observed Dust Ring Properties as Probes of Planet Masses
Article Publication Date
28-May-2026
Red dwarf stars detected 'eating' Earth-like planets
image:
This artist's impression shows two Earth-sized worlds passing in front of their parent red dwarf star in the TRAPPIST-1 system 40 light-years away.
view moreCredit: ESA/Hubble
Astronomers have found some of the strongest evidence yet that stars can swallow their own planets.
A new study, published in Monthly Notices of the Astronomical Society, supports the long-held belief that young stars are capable of 'eating' nearby worlds as planetary systems form.
Researchers from Keele University and the University of Exeter studied thousands of stars and found evidence that six different red dwarfs – the smallest, coolest, and most common type of star in the universe – had engulfed Earth-like rocky planets.
What gave it away was the highly detectable chemical 'fingerprint', said lead author Professor Robin Jeffries, from Keele University.
"We found that a few of the red dwarf stars we studied contained lithium, a chemical element that should not be there," he explained.
"Therefore even a small amount of lithium stands out clearly in these stars – a bit like throwing paint onto a blank canvas."
Professor Jeffries added: "Red dwarfs are smaller and cooler than our Sun but inside they are extremely hot. This heat should destroy all of their fragile lithium in nuclear reactions shortly after they form."
Because of this, there have been previous predictions that finding the presence of lithium in their atmospheres could signpost the engulfment of still lithium-rich material accreted from a surrounding planetary system.
In the new study, the researchers looked at young star clusters using spectroscopic data, which refers to the study of how different matter interacts with electromagnetic radiation.
The Gaia-ESO Spectroscopic (GES) survey data covered thousands of stars, of which the team identified six different red dwarfs in three separate clusters which had much higher lithium content than other stars of a similar spectral type.
Their analysis suggests that these stars had dramatically ‘swallowed’ their surrounding Earth-like planets, or about 3 to 10 Earth-masses of planetary material in total, providing a fresh burst of lithium to their otherwise lithium-depleted atmospheres.
These engulfment events have long been theorised as a possible and even probable outcome during early planetary system formation, and may even have happened earlier in our own Solar System.
If this explanation proves correct, a new window will have been opened into the early lives of planetary systems, allowing the quantity and timing of planetary engulfment to be investigated.
Unlike isolated stars, those found in clusters have well-understood ages and masses, and the presence of many similar siblings, born from the same initial material, means even small chemical abundance differences are easier to establish, the researchers said.
ENDS
Media contacts
Sam Tonkin
Royal Astronomical Society
Mob: +44 (0)7802 877 700
Science contacts
Professor Robin Jeffries
Keele University
r.d.jeffries@keele.ac.uk
Images & captions
Caption: This artist's impression shows two Earth-sized worlds passing in front of their parent red dwarf star in the TRAPPIST-1 system 40 light-years away.
Credit: ESA/Hubble
Further information
The paper ‘Lithium-rich M-dwarfs at the ZAMS: evidence for planetary engulfment?’ by Jeffries et al. has been published in Monthly Notices of the Royal Astronomical Society. DOI: 10.1093/mnras/stag815.
Notes for editors
About the Royal Astronomical Society
The Royal Astronomical Society (RAS), founded in 1820, encourages and promotes the study of astronomy, solar-system science, geophysics and closely related branches of science.
The RAS organises scientific meetings, publishes international research journals, recognises outstanding achievements by the award of medals and prizes, maintains an extensive library, supports education through grants and outreach activities and represents UK astronomy nationally and internationally. Its more than 4,000 members (Fellows), a third based overseas, include scientific researchers in universities, observatories and laboratories as well as historians of astronomy and others.
The RAS accepts papers for its journals based on the principle of successful peer review, following which experts on the Editorial Boards accept the papers for publication. The Society issues press releases based on a similar principle, but the organisations and scientists concerned have overall responsibility for their content.
Keep up with the RAS on Instagram, Bluesky, LinkedIn, Facebook and YouTube.
Download the RAS Supermassive podcast
Journal
Monthly Notices of the Royal Astronomical Society
Article Title
‘Lithium-rich M-dwarfs at the ZAMS: evidence for planetary engulfment?’
Article Publication Date
28-May-2026
Scientists show how baby stars’ cradles get their radial shape
New 3D simulations show a dying star's last shockwave can weave a star-forming hub into shape
image:
The left panel shows a hub-filament system observed in an actual star-forming region; the right shows the structure produced by this study's 3D simulation. Both show multiple elongated filaments of gas radiating toward a dense central hub. The study shows that this characteristic pattern can emerge when a fast interstellar shockwave strikes a molecular cloud with a curved magnetic field.
view moreCredit: Left: M. S. N. Kumar, ESA/Herschel, NASA/JPL-Caltech (Spitzer); Right: S. Nozaki & S. Inutsuka
Fukuoka, Japan—The universe is full of fascinating structures, and some of the most striking take shape inside the giant clouds where stars are born. There, streams of gas appear to converge from all directions toward a dense central hub, like spokes meeting at the center of a wheel.
Now, researchers from Kyushu University and Nagoya University have used 3D computer simulations to reveal the physics behind these elegant structures. The study was published in March 2026 in The Astrophysical Journal Letters.
“Stars are born inside molecular clouds—vast, cold clouds of gas that drift through space,” says Shingo Nozaki, a doctoral student at Kyushu University's Graduate School of Sciences, and a Research Fellow of the Japan Society for the Promotion of Science (JSPS). “But they only form in the coldest and densest parts of those stellar nurseries, where gas can collapse under its own gravity. In some of these star-forming regions, gas is organized into characteristic hub-and-spoke patterns known as Hub-Filament Systems (HFS).”
How this radial pattern forms, however, has long remained unclear. At a workshop at Kyushu University last summer, Nozaki and Shu-ichiro Inutsuka of Nagoya University began exploring one possible explanation: what happens when an external shock hits a gas cloud with a pinched magnetic field shape?
Using ATERUI III, an astronomy-dedicated supercomputer operated by the National Astronomical Observatory of Japan, they conducted a 3D magnetohydrodynamic simulation, a computational method that models how gas and magnetic fields evolve together over time.
As a rough analogy, Nozaki pictures the initial molecular cloud as a dorayaki—a Japanese pancake that's thick in the middle and thin at the edges. A vertical magnetic field runs through the cloud, while gravity pulls the field inward at the center, bending it into an hourglass shape. The team then introduced a cosmic disturbance into the cloud, mimicking the kind of disturbance triggered by a supernova remnant or by expanding gas around massive stars.
The results show several elongated structures that develop toward a dense central region, closely resembling observed HFSs. As the magnetic field lines curve inward, the shock wave strikes different parts of the cloud at different angles, creating what physicists call oblique shocks. These shocks strengthen parts of the magnetic field, forming invisible channels that guide compressed gas into long, narrow filaments converging toward the center.
The simulation also revealed that gas does not flow uniformly into the hub. Dense gas within the filaments moves steadily inward, accelerating as it approaches the center, while the low-density gas between filaments stays mostly still. This indicates that the main carriers of mass to the central region are the shock-produced dense filaments, not the cloud as a whole, offering insights into why star formation efficiency remains limited to a few percent.
The team notes that this study focused on a geometrically regular type of HFS, while many observed systems are more asymmetric and complex. Next, they plan to systematically vary the shock direction and strength; the cloud’s density structure; and the magnetic field geometry. This will help them connect different cloud environments to the formation of various massive stars and clusters, and more broadly, to understand how star formation proceeds across galaxies.
“There are two main sources of these shock waves: radiation-driven ‘bubbles’ from newly formed massive stars, and expanding supernova remnants formed when a massive star reaches the end of its life,” adds Nozaki. “There is something almost like a life cycle in this. What a star leaves behind can go on to shape the next cradle of stars.”
###
For more information about this research, see " An Origin of Radially Aligned Filaments in Hub-filament Systems," Shingo Nozaki and Shu-ichiro Inutsuka, The Astrophysical Journal Letters, https://doi.org/10.3847/2041-8213/ae4c84
About Kyushu University
Founded in 1911, Kyushu University is one of Japan's leading research-oriented institutions of higher education, consistently ranking as one of the top ten Japanese universities in the Times Higher Education World University Rankings and the QS World Rankings. Located in Fukuoka, on the island of Kyushu—the most southwestern of Japan’s four main islands—Kyushu U sits in a coastal metropolis frequently ranked among the world’s most livable cities and historically known as Japan’s gateway to Asia. Its multiple campuses are home to around 19,000 students and 8,000 faculty and staff. Through its VISION 2030, Kyushu U will “drive social change with integrative knowledge.” By fusing the spectrum of knowledge, from the humanities and arts to engineering and medical sciences, Kyushu U will strengthen its research in the key areas of decarbonization, medicine and health, and environment and food, to tackle society’s most pressing issues.
The left panel shows a hub-filament system observed in an actual star-forming region; the right shows the structure produced by this study's 3D simulation. Both show multiple elongated filaments of gas radiating toward a dense central hub. The study shows that this characteristic pattern can emerge when a fast interstellar shockwave strikes a molecular cloud with a curved magnetic field.
Credit
Shingo Nozaki / Kyushu University
Journal
The Astrophysical Journal Letters
Method of Research
Computational simulation/modeling
Subject of Research
Not applicable
Article Title
An Origin of Radially Aligned Filaments in Hub-filament Systems
WVU researcher finds a surprising phenomenon in NASA data from Mars
image:
Christopher Fowler, a WVU planetary scientist, is part of a NASA research team that analyzes data collected from Mars by the twin satellites of the MAVEN mission.
view moreCredit: WVU Photo/Matt Sunday
Data beamed back from Mars by the NASA spacecraft MAVEN provides the first evidence that a phenomenon protecting planets from solar winds can occur in the atmospheres of worlds that lack strong magnetic fields, according to research led by West Virginia University planetary scientist Christopher Fowler.
Fowler, a research assistant professor at the WVU Eberly College of Arts and Sciences and a member of the WVU Center for Kinetic Plasma Physics, said MAVEN’s observations advance scientists’ understanding of how the sun interacts with the solar system and especially with unmagnetized bodies like comets, Saturn’s moon Titan, Venus and Mars.
Fowler and his colleagues discovered indications of a phenomenon called the Zwan-Wolf effect in data MAVEN collected in December 2023, during a “coronal mass ejection event” in which huge magnetic clouds of electrified gas called plasma exploded from the sun and spread through the solar system, causing solar storms and electromagnetic disturbances.
Their findings appear in Nature Communications.
When solar wind, the continuous flow of plasma emitted by the sun, encounters bodies such as planets and comets, it is deflected around them, much like the flow of water in a stream is deflected around a rock, Fowler explained.
“However,” he added, “because the water in that stream is relatively dense, physical collisions between water molecules bumping into each other and the rock determine how the water is diverted. In contrast, the environment in space is so tenuous that solar wind particles do not bump into each other. Instead, electromagnetic forces control how particles are deflected around these bodies.”
If the solar wind meets and curves around a planet that has a strong magnetic field, like Earth, that’s when the Zwan-Wolf effect plays a role, contributing to those electromagnetic forces by squeezing the plasma through “magnetic flux tubes” — regions of space created by bundles of parallel magnetic field lines.
“The squeezing helps move the solar wind plasma around the planet, and it makes the plasma less dense in front of the planet,” Fowler said.
“By finding this effect in the atmosphere of Mars, we are discovering new ways in which our sun can interact with and affect planets in our solar system. It’s amazing to think that an eruption on the sun can disturb the atmosphere of Mars 142 million miles away.”
Before Fowler noticed what he called “very interesting wiggles” in the observations from MAVEN, scientists believed the Zwan-Wolf effect only happened in the region above a planet’s atmosphere, known as the magnetosphere.
What Fowler’s research group discovered in the data from the 2023 solar storm was the first evidence of the Zwan-Wolf effect happening not in a planetary magnetosphere, but in Mars’ atmosphere.
“We think this effect could occur in the Martian atmosphere all the time, but it’s usually such a small effect that our instruments aren’t sensitive enough to detect it,” Fowler said.
“The solar storm really hit Mars hard and disturbed the entire space environment around the planet. This seems to have amplified the Zwan-Wolf effect so that we could observe it during this time period. We got lucky, being in the right place at the right time with MAVEN to see this.”
Questions remain, he added, including how far down into the Martian atmosphere the Zwan-Wolf effect can reach.
“We observed these signatures all the way down to the lowest altitudes that MAVEN sampled, suggesting that it impacted the atmosphere even below the spacecraft,” Fowler said. “Understanding how these space weather events impact our solar system is important, not only for keeping our robotic — and potentially, human — explorers safe in the future, but for protecting the space assets that we rely on for our everyday technology here on Earth.”
Journal
Nature Communications
Article Title
Detection of Zwan-Wolf effect in the ionosphere of Mars
Article Publication Date
18-May-2026
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