NASA selected a mission concept to research how space weather and dynamics within Earth’s atmosphere influence the space environment and help improve prediction capabilities for impacts on crucial technology, such as GPS and low Earth orbit satellites, as well as astronauts in space.

The DAPHNE (Dynamic Atmosphere-Ionosphere Explorer) mission will enter Phase B of development, which includes planning and design for flight and mission operations. It will use identical twin satellites to study how changes in Earth’s lower atmosphere influence our planet’s upper atmosphere, where space weather is manifested.

“NASA is advancing the United States’ leadership as a space weather-ready nation, and by providing new insights into Earth’s atmosphere we can better predict and prepare for impacts in our daily lives on Earth and in space,” said Nicky Fox, associate administrator, Science Mission Directorate, NASA Headquarters in Washington. “As NASA sends astronauts beyond Earth’s magnetic protection to the Moon, Mars, and beyond, DAPHNE will join the NASA science fleet strategically located across the solar system to provide data that will help mission planners predict and mitigate the effects of space weather for the benefit of all.”

The DAPHNE mission’s low-risk high-return concept will provide coordinated, multi-point measurements of neutral winds, temperature, and composition in the thermosphere. The ionosphere and thermosphere regions are where Earth’s neutral atmosphere transitions into the ionized plasma of space. In this thin shell that surrounds the planet, the atmosphere is in constant motion, shaped by the influence of solar activity and changes in the lower atmosphere and in near-Earth space.

Fundamental observations and physical insights from the DAPHNE mission will incorporate lower-atmospheric energy data to advance space weather predictive capabilities. The mission is led by Aimee Merkel from the Laboratory for Atmospheric and Space Physics at the University of Colorado, Boulder.

The mission will be subject to a confirmation review in 2027, which will assess the progress of the mission and the availability of funds. If confirmed, the total estimated cost of the mission, excluding launch, will not exceed $250 million in fiscal year 2023 dollars, with a mission launch date of no earlier than 2029.

The DAPHNE mission was proposed as a concept study in response to the DYNAMIC (Dynamical Neutral Atmosphere-Ionosphere Coupling) mission announcement of opportunity. Funding and management oversight for this mission is provided by the Solar Terrestrial Probes program at NASA’s Goddard Space Flight Center in Greenbelt, Maryland.

For more information on NASA’s heliophysics missions, visit:

https://science.nasa.gov/heliophysics

-end-

Abbey Interrante / Karen Fox
Headquarters, Washington
202-358-1600
abbey.a.interrante@nasa.gov / karen.c.fox@nasa.gov

Physicists with LHCb Collaboration at CERN’s Large Hadron Collider (LHC) have detected the elusive Ωcc⁺ baryon, a particle containing two charm quarks and one strange quark, completing a long-sought family of doubly charmed baryons first predicted over half a century ago.

The post CERN Physicists Discover Third and Final Member of Doubly Charmed Baryon Family appeared first on Sci.News: Breaking Science News.

Physicists have revealed that the unusual decay of an “exotic” subatomic particle could offer new clues to its mysterious structure.

The discovery, reported by a team of physicists in a study published in Physical Review Letters, argues that it provides the first “crucial discrimination” between current theoretical models of a variety of subatomic particles known as the Ds(2317) meson.

Exotic Subatomic Mysteries

The new research has its beginnings more than two decades ago, with the initial detection of an unusual particle known as the Ds(2317) meson. Part of what makes this particle unique is the fact that it possesses one charm quark (or “c quark,” a kind of elementary particle) and one strange antiquark—the third lightest of all the known quarks.

It was deemed a major discovery at the time, and for good reason: it seemed to point at a significant discrepancy between the particle’s measured mass of 2.317 GeV/c2, and predictions based on estimates that placed it significantly higher, at around 2.4 GeV/c2.

Now, in a new study by researchers with the Belle and Belle II Collaboration, observations of previously undetected behaviors that include never-before-seen light-emissions during the particle’s decay have been described for the first time.

Based on their analysis, the team believes their new findings mark not only a significant first in the study of these particles, but that they may also help researchers solve the longstanding mystery involving apparent discrepancies between the observed and expected mass values for the Ds(2317) meson.

The findings, the team says, could also provide physicists with deeper insights into the fundamental forces that currently bind matter.

Unraveling a Baffling Discrepancy

The team approached the problem by first proposing a range of different models that could potentially describe the internal structure of the Ds(2317) meson. Of key importance was the fact that each of the different models allows researchers to predict a specific range of potential values for the particle’s decay.

This was achieved based on the probability that the Ds(2317 meson will decay by emitting a gamma ray, which was then divided by an entirely separate probability: that the particle would emit a pion—a type of meson with a mass roughly 270 times that of an electron—rather than a gamma ray.

Based on these two possibilities, the team determined that measurements indicating a ratio of greater than 8.1% would point to the likelihood that the meson represents a compact state involving quark-antiquark models.

However, if the calculated value turned out to be lower—specifically in the range of between 0.5% and 4.25%—that would instead favor models that describe the particle as functioning closer to being a sort of molecule-like state of two separate mesons.

Well Above Standard Deviations

With such values in mind, the team then went to work to determine which was more likely with help from data collected by the Japanese KEKB and SuperKEKB electron–positron colliders.

Using this information, the particle’s gamma-emitting decay was successfully detected, revealing a statistical significance above ten standard deviations. Next, the Belle and Belle II Collaboration conducted measurements that showed the decay ratio between photons and pions was close to 7%, placing the determined value smaller than the majority of quark-antiquark models, and at a greater value than those in the molecular models.

“This result provides crucial discrimination between theoretical models of the Ds(2317) structure,” the team writes.

Going forward, the researchers believe additional insights that may help to conclusively reveal the mysterious Ds(2317) meson’s structure may be achievable through more complete measurements of the particle’s decay rate.

The recent paper, “Observation of the Radiative Decay 𝐷*𝑠0(2317)+→𝐷*𝑠+𝛾,” appeared in Physical Review Letters.

Micah Hanks is the Editor-in-Chief and Co-Founder of The Debrief. A longtime reporter on science, defense, and technology with a focus on space and astronomy, he can be reached at micah@thedebrief.org. Follow him on X @MicahHanks, and at micahhanks.com.

Scientists from Asia Pacific’s largest paint and coating manufacturer have developed a new “ultra-black” automotive coating using carbon nanotubes that absorbs over 99% of the light it receives, resulting in the darkest black of any currently available paint or coating.

The NIPSEA Group’s research team said its new ultra-black coating, which they describe as “deep, jet black,” meets stringent automotive standards, a critical requirement in markets like China, where trendy, luxury vehicles in the darkest colors are in high demand.

Carbon Nanotubes Absorb Light to Create Darkest Black “Ultra-Black” Coating

According to a statement announcing the new ultra-black coating, BMW first introduced a concept car in 2019 with a vertically aligned carbon nanotube (VACNT) array outer coating. Due to the unique material properties of carbon nanotubes, including the ability to bend or absorb light, the researchers said that its introduction “set off a race” among auto manufacturers to create a similar, ‘black hole’ effect with a pronounced dark appearance. 

“Automotive coating companies have been actively pursuing innovations in color technology to develop mass-processable ultra-black coating solutions with extreme blackness,” explained Zhiwei Liu, a research chemist with the company’s Color Technology Group, Core R&D, and an author on the study outlining the new coating.

The researchers note that ultra-black coatings are in unusually high demand in Asian countries, where having the darkest vehicle can represent a status symbol. has become a “key selling point” in China.

“Deep black finishes have long been the premium choice and signature color for luxury cars due to their elegant appearance, powerful visual impact, and luxurious undertone,” the researcher explained.

Although scientists have explored more practical ways to achieve the desired ultra-black effect, the new research once again leverages the unusual properties of carbon nanotubes to create an ultra-black coating that is darker than even the darkest commercially available alternative.

Creating a Stable Composite That Meets Automotive Standards

According to the team’s statement, they began by exploring methods to combine the benefits of carbon nanotubes with a black pigment that would serve as the coating’s color base. Critically, the team needed to create a nano-sized carbon black pigment-carbon nanotube composite that was also stable at a wide range of temperatures. and moisture conditions.

After exploring several formulations, Liu and colleagues succeeded in a stable nanotube-pigment composite. Next, the team incorporated the new carbon nanotube-based mixture into a coating binder and sprayed it onto a model car.

Because the new ultra-black coating uses structural absorption of light rather than the carbon black dispersion method used in current approaches, tests revealed an average absorption of 99.90% across all visible wavelengths. The team said its new coating also displayed “excellent long-term stability” during water and humidity tests.

Although the light absorption levels set a new standard for the darkest achievable automotive coating, Liu said advancements in dispersing technology and equipment leave his team “room for improvements.” The researcher highlighted potential advancements in “practical processability of carbon-nanotube-containing nanomaterials.”

Liu and colleagues also noted that increasing the proportion of carbon nanotubes in the material could further increase its light-absorbing capacity. However, they conceded, this approach “would also bring difficulties in industrial-grade processability.”

Future Improvements Include Even Darker Multi-Layer Options

When discussing potential future improvements, the team said scientists could fabricate multilayered ultra-black coatings. In theory, they note that this approach could result in a “gradient refractive index that reduces interface reflection and further enhances light absorption efficiency,” producing an even darker look than their single-layer version.

Although the ultra-black automotive coating is not yet commercially available, the team said they have already completed a “proof of concept” manufacturing design. Still, they conceded, given technical and regulatory challenges that remain, “it may still be a while before ultra-black cars made with this film will be able to hit the road.”

“Further efforts will focus on the verification of coating application window and the comprehensive film performance validations of carbon black pigment-carbon nanotube composite-based ultra-black automotive coating,” Liu concluded.

The study “Robust ultra-black automotive coating with structural absorption and high absorption efficiency based on waterborne carbon black/CNT composite” was published in Matter & Light.

Christopher Plain is a Science Fiction and Fantasy novelist and Head Science Writer at The Debrief. Follow and connect with him on X, learn about his books at plainfiction.com, or email him directly at christopher@thedebrief.org.

This NASA Hubble Space Telescope image features a galaxy cluster, called CL0016+1609 or MACS J0018.5+1626, that is very bright at X-ray wavelengths and is one of the most extensively studied clusters at X-ray and radio wavelengths. The X-ray observations of this cluster revealed that it is two clusters merging along our line of sight.

Researchers requested time to observe CL0016+1609 with Hubble’s Advanced Camera for Surveys because that data would help them accurately measure the cluster’s dark-matter distribution, which helps them study the merger and the role of CL0016+1609 in the large-scale structure of the universe. Hubble can’t directly see dark matter, but its infrared and visible light observations can detect dark matter’s gravitational lensing effects on the normal matter Hubble observes.

The data in this image also includes observations with Hubble’s Wide Field Camera 3 taken as part of an observing program that obtained the first Hubble infrared images of 46 massive galaxy clusters and looked for distant galaxies gravitationally lensed by these clusters. Called RELICS (Reionization Lensing Cluster Survey), this survey found some 300 high-redshift candidate galaxies lensed by these clusters.

You can see the faint vertical arc of one of these distant galaxies in the image above. Look for it just to the left of the large elliptical galaxies in the center of the image. Another brighter, though shorter arc is visible just above and to the right of the large elliptical galaxies in the center of the image.

Media Contact:

Claire Andreoli
NASA’s Goddard Space Flight Center, Greenbelt, MD
claire.andreoli@nasa.gov

A new study of two supernova remnants, the debris left behind after stars explode, suggests the explosions came from stellar siblings that once orbited each other. The first star’s detonation sent its binary companion hurtling through space, and then, after traveling for thousands of years, the surviving star blew up too.

“Using 16 years of data from NASA’s Fermi Gamma-ray Space Telescope, our analysis uncovered gamma rays associated with a supernova remnant that was hidden in the glare of its neighbor, the Jellyfish Nebula, one of the brightest gamma-ray-emitting supernova remnants known,” said Miltiadis Michailidis, a postdoctoral fellow in the physics department at Stanford University in California. “There are so many striking connections between the two remnants that we conclude they’re likely related, giving us the first known example of a binary system where both stars have undergone supernova explosions.”

Michailidis presented the findings Wednesday at the 248th meeting of the American Astronomical Society in Pasadena, California. A paper describing the results will appear in a future edition of Nature Communications.

The study focused on a faint supernova remnant called G189.6+3.3, which is mainly visible in X-rays. It is upstaged by its brighter and better-known neighbor, the Jellyfish Nebula (IC 443). The two star wrecks, both located in the constellation Gemini, appear to partially overlap as seen in X-rays. Recent X-ray evidence suggests that hot plasma likely associated with G189.6+3.3 may extend across the entire region, a hint that the overlap may be nearly total.

A massive star explodes when its energy-producing core runs out of fuel and collapses under its own weight, triggering an explosion that blows the star apart. The explosion’s shock wave encloses a hot cloud of debris that rapidly expands into space. So far, astronomers have cataloged about 300 supernova remnants in our galaxy.  

The Fermi mission is part of NASA’s fleet of observatories monitoring the changing cosmos to help humanity better understand how the universe works. More than a decade ago, observations from Fermi’s LAT (Large Area Telescope) showed that the shock waves of supernova remnants accelerated particles to within a fraction of the speed of light, a process first proposed by physicist Enrico Fermi — the mission’s namesake — in 1949.

These high-speed particles, called cosmic rays, interact with interstellar gas to produce gamma rays, the highest-energy form of light. Protons make up 99% of cosmic ray particles. To prove that accelerated protons are responsible for the glow, astronomers search for a specific gamma-ray feature. When cosmic-ray protons smash into interstellar gas, they produce a short-lived particle called a neutral pion, which almost immediately decays into a pair of gamma rays. This emission occurs within a specific band of energies associated with the neutral pion’s mass and lies within the range detected by Fermi’s LAT instrument.

In 2013, Fermi observations proved that the Jellyfish Nebula, which is interacting with part of a glowing cloud of hydrogen gas known as Sharpless 249, produced gamma rays through this mechanism. Its neighbor, G189.6+3.3, was discovered in 1994 as part of an X-ray survey by the German-led ROSAT (Roentgen Satellite) mission.

A bright filament of gas lies between the overlapping remnants. New observations of this feature reveal that the shock wave from G189.6+3.3 slammed into dense interstellar gas there and dramatically slowed, key evidence that both remnants are interacting with the same cloud system.

Astronomers think the Jellyfish Nebula is also a candidate PeVatron, a cosmic particle accelerator capable of boosting protons to energies so high they could nearly escape our galaxy. Such particles can produce gamma rays with trillions of times more energy than visible light. Finding a second particle accelerator near the Jellyfish Nebula could offer scientists new clues for how supernova remnants develop into PeVatrons.

“The overlapping remnants, a connecting gas filament, and the availability of data from Fermi and other facilities motivated us to delve into this complex but little-studied region,” said co-author Marianne Lemoine-Goumard, an astrophysicist at the French National Centre for Scientific Research (CNRS) based at the University of Bordeaux. “With Fermi’s LAT instrument, we found gamma-ray emission associated with accelerated protons in the northern part of the fainter remnant. If both remnants are interacting with the same structure, then they must share a common distance from us.”

The team concludes the remnants lie about 6,000 light-years away, their explosion centers are separated by roughly 40 light-years projected onto the plane of the sky, and the original stars may have been 20 or more times the Sun’s mass.

Estimates of the remnants’ ages vary widely, but the team concludes that the age of the Jellyfish Nebula is 8,000 to 9,000 years, while G189.6+3.3 is between 20,000 to 110,000 years old. This means the delay between the explosions could have extended for up to 100,000 years.

In addition, the team conducted computer simulations of a million massive binary systems. They show that systems where the stars orbit close enough to exchange matter and interact during their lives can readily produce dual supernova explosions with similar separations and time delays as those found for the remnants. The team also estimated that the chance of randomly encountering this combination of observed spatial alignment and compatible distances to be less than 1%, strongly supporting a physical association.

“The evidence we’ve compiled — including observations across the spectrum, the chemical and physical properties of the remnants, simulations, and more — paints a compelling picture of a dual supernova event,” said Michailidis.

This study identifies a unique possible example of a binary system where both stars exploded as supernovae and left behind separate, detectable supernova remnants. Astronomers think that most massive stars form in binary or multiple-star systems. The Jellyfish Nebula/G189.6+3.3 complex offers astronomers a rare opportunity to study how massive binary stars evolve, exchange matter, explode, and experience velocity changes — called kicks — induced by the supernova blast. It also provides a powerful new laboratory for understanding how coupled supernova remnants behave, including how they accelerate particles, generate gamma rays, and shape their surrounding environments.

“Fermi’s gamma-ray observations of supernova remnants continue to reveal the dynamic lives of stars,” said Elizabeth Hays, the Fermi project scientist at NASA’s Goddard Space Flight Center in Greenbelt, Maryland. “We can now connect the glowing remains of two massive stars to a powerful pair that evolved together over thousands of years.”

By Francis Reddy
NASA’s Goddard Space Flight Center, Greenbelt, Md.

Media Contact:
Claire Andreoli
301-286-1940
NASA’s Goddard Space Flight Center, Greenbelt, Md.

This NASA Hubble Space Telescope image features a galaxy cluster, called CL0016+1609 or MACS J0018.5+1626, that is very bright at X-ray wavelengths and is one of the most extensively studied clusters at X-ray and radio wavelengths. The X-ray observations of this cluster revealed that it is two clusters merging along our line of sight.

Researchers requested time to observe CL0016+1609 with Hubble’s Advanced Camera for Surveys because that data would help them accurately measure the cluster’s dark-matter distribution, which helps them study the merger and the role of CL0016+1609 in the large-scale structure of the universe. Hubble can’t directly see dark matter, but its infrared and visible light observations can detect dark matter’s gravitational lensing effects on the normal matter Hubble observes.

The data in this image also includes observations with Hubble’s Wide Field Camera 3 taken as part of an observing program that obtained the first Hubble infrared images of 46 massive galaxy clusters and looked for distant galaxies gravitationally lensed by these clusters. Called RELICS (Reionization Lensing Cluster Survey), this survey found some 300 high-redshift candidate galaxies lensed by these clusters.

You can see the faint vertical arc of one of these distant galaxies in the image above. Look for it just to the left of the large elliptical galaxies in the center of the image. Another brighter, though shorter arc is visible just above and to the right of the large elliptical galaxies in the center of the image.

Media Contact:

Claire Andreoli
NASA’s Goddard Space Flight Center, Greenbelt, MD
claire.andreoli@nasa.gov

The post Hubble Glimpses Merging Galaxy Clusters appeared first on NASA Science.

A new study suggests that the collapse of a massive star could spark the creation of a tiny expanding universe rather than a black hole. The resulting object, called a gravastar, would avoid the singularity and event horizon that make black holes so puzzling. Massive stars produce light and heat through nuclear fusion in their [...]

Quantum computing news usually picks up near the end of the year, as companies try to provide evidence that they are hitting benchmarks on time. However, there have been interesting announcements as the summer starts this year, from incremental progress to attention-grabbing promises. As we did earlier this month, Ars has a rundown of some of the most significant announcements.

These include a promise of useful, error-corrected quantum computing as soon as 2028, details on an updated trapped ion processor, and a case in which claims of quantum supremacy have been cut back a bit thanks to advances in more traditional algorithms.

2028 is remarkably soon

Many people in the field expect that useful quantum computers are still about five to 10 years away. While there may be a few useful algorithms that can be run on existing error-prone hardware, almost all of the interesting problems that quantum computing can be applied to will require some form of error correction enabled by linking a small collection of hardware qubits together into what's called a logical qubit. Logical qubits include the redundant storage of information along with neighboring qubits that can be measured to determine when errors occur and how to fix them.

Read full article

Comments

© QuEra

Quantum computing news usually picks up near the end of the year, as companies try to provide evidence that they are hitting benchmarks on time. However, there have been interesting announcements as the summer starts this year, from incremental progress to attention-grabbing promises. As we did earlier this month, Ars has a rundown of some of the most significant announcements.

These include a promise of useful, error-corrected quantum computing as soon as 2028, details on an updated trapped ion processor, and a case in which claims of quantum supremacy have been cut back a bit thanks to advances in more traditional algorithms.

2028 is remarkably soon

Many people in the field expect that useful quantum computers are still about five to 10 years away. While there may be a few useful algorithms that can be run on existing error-prone hardware, almost all of the interesting problems that quantum computing can be applied to will require some form of error correction enabled by linking a small collection of hardware qubits together into what's called a logical qubit. Logical qubits include the redundant storage of information along with neighboring qubits that can be measured to determine when errors occur and how to fix them.

Read full article

Comments

© QuEra

A new study of two supernova remnants, the debris left behind after stars explode, suggests the explosions came from stellar siblings that once orbited each other. The first star’s detonation sent its binary companion hurtling through space, and then, after traveling for thousands of years, the surviving star blew up too.

“Using 16 years of data from NASA’s Fermi Gamma-ray Space Telescope, our analysis uncovered gamma rays associated with a supernova remnant that was hidden in the glare of its neighbor, the Jellyfish Nebula, one of the brightest gamma-ray-emitting supernova remnants known,” said Miltiadis Michailidis, a postdoctoral fellow in the physics department at Stanford University in California. “There are so many striking connections between the two remnants that we conclude they’re likely related, giving us the first known example of a binary system where both stars have undergone supernova explosions.”

Michailidis presented the findings Wednesday at the 248th meeting of the American Astronomical Society in Pasadena, California. A paper describing the results will appear in a future edition of Nature Communications.

The study focused on a faint supernova remnant called G189.6+3.3, which is mainly visible in X-rays. It is upstaged by its brighter and better-known neighbor, the Jellyfish Nebula (IC 443). The two star wrecks, both located in the constellation Gemini, appear to partially overlap as seen in X-rays. Recent X-ray evidence suggests that hot plasma likely associated with G189.6+3.3 may extend across the entire region, a hint that the overlap may be nearly total.

A massive star explodes when its energy-producing core runs out of fuel and collapses under its own weight, triggering an explosion that blows the star apart. The explosion’s shock wave encloses a hot cloud of debris that rapidly expands into space. So far, astronomers have cataloged about 300 supernova remnants in our galaxy.  

The Fermi mission is part of NASA’s fleet of observatories monitoring the changing cosmos to help humanity better understand how the universe works. More than a decade ago, observations from Fermi’s LAT (Large Area Telescope) showed that the shock waves of supernova remnants accelerated particles to within a fraction of the speed of light, a process first proposed by physicist Enrico Fermi — the mission’s namesake — in 1949.

These high-speed particles, called cosmic rays, interact with interstellar gas to produce gamma rays, the highest-energy form of light. Protons make up 99% of cosmic ray particles. To prove that accelerated protons are responsible for the glow, astronomers search for a specific gamma-ray feature. When cosmic-ray protons smash into interstellar gas, they produce a short-lived particle called a neutral pion, which almost immediately decays into a pair of gamma rays. This emission occurs within a specific band of energies associated with the neutral pion’s mass and lies within the range detected by Fermi’s LAT instrument.

In 2013, Fermi observations proved that the Jellyfish Nebula, which is interacting with part of a glowing cloud of hydrogen gas known as Sharpless 249, produced gamma rays through this mechanism. Its neighbor, G189.6+3.3, was discovered in 1994 as part of an X-ray survey by the German-led ROSAT (Roentgen Satellite) mission.

A bright filament of gas lies between the overlapping remnants. New observations of this feature reveal that the shock wave from G189.6+3.3 slammed into dense interstellar gas there and dramatically slowed, key evidence that both remnants are interacting with the same cloud system.

Astronomers think the Jellyfish Nebula is also a candidate PeVatron, a cosmic particle accelerator capable of boosting protons to energies so high they could nearly escape our galaxy. Such particles can produce gamma rays with trillions of times more energy than visible light. Finding a second particle accelerator near the Jellyfish Nebula could offer scientists new clues for how supernova remnants develop into PeVatrons.

“The overlapping remnants, a connecting gas filament, and the availability of data from Fermi and other facilities motivated us to delve into this complex but little-studied region,” said co-author Marianne Lemoine-Goumard, an astrophysicist at the French National Centre for Scientific Research (CNRS) based at the University of Bordeaux. “With Fermi’s LAT instrument, we found gamma-ray emission associated with accelerated protons in the northern part of the fainter remnant. If both remnants are interacting with the same structure, then they must share a common distance from us.”

The team concludes the remnants lie about 6,000 light-years away, their explosion centers are separated by roughly 40 light-years projected onto the plane of the sky, and the original stars may have been 20 or more times the Sun’s mass.

Estimates of the remnants’ ages vary widely, but the team concludes that the age of the Jellyfish Nebula is 8,000 to 9,000 years, while G189.6+3.3 is between 20,000 to 110,000 years old. This means the delay between the explosions could have extended for up to 100,000 years.

In addition, the team conducted computer simulations of a million massive binary systems. They show that systems where the stars orbit close enough to exchange matter and interact during their lives can readily produce dual supernova explosions with similar separations and time delays as those found for the remnants. The team also estimated that the chance of randomly encountering this combination of observed spatial alignment and compatible distances to be less than 1%, strongly supporting a physical association.

“The evidence we’ve compiled — including observations across the spectrum, the chemical and physical properties of the remnants, simulations, and more — paints a compelling picture of a dual supernova event,” said Michailidis.

This study identifies a unique possible example of a binary system where both stars exploded as supernovae and left behind separate, detectable supernova remnants. Astronomers think that most massive stars form in binary or multiple-star systems. The Jellyfish Nebula/G189.6+3.3 complex offers astronomers a rare opportunity to study how massive binary stars evolve, exchange matter, explode, and experience velocity changes — called kicks — induced by the supernova blast. It also provides a powerful new laboratory for understanding how coupled supernova remnants behave, including how they accelerate particles, generate gamma rays, and shape their surrounding environments.

“Fermi’s gamma-ray observations of supernova remnants continue to reveal the dynamic lives of stars,” said Elizabeth Hays, the Fermi project scientist at NASA’s Goddard Space Flight Center in Greenbelt, Maryland. “We can now connect the glowing remains of two massive stars to a powerful pair that evolved together over thousands of years.”

By Francis Reddy
NASA’s Goddard Space Flight Center, Greenbelt, Md.

Media Contact:
Claire Andreoli
301-286-1940
NASA’s Goddard Space Flight Center, Greenbelt, Md.

The post NASA’s Fermi Mission Uncovers Possible Sibling Supernova Remnants appeared first on NASA Science.

Future interstellar travelers who hope to reach distant star systems will likely need better propulsion technologies than the chemical rockets humans currently rely on for our exploration of space.

Among the range of proposed alternatives, one potential candidate involves what are called solar light sails, a theoretical propulsion system that relies on pressure generated from solar radiation against a large surface to move a spacecraft.

Such concepts have been proposed since the 1980s, some of which combine the idea of using sunlight as a power source with the implementation of lasers, which could propel such futuristic starships to speeds our best current technologies cannot attain.

However, not all spacecraft propulsion experts are necessarily sold on the idea of solar light sails just yet. According to new findings detailed in a paper by researchers Jiaze Li and Chao Shen of the Harbin Institute of Technology in China, this novel form of propulsion may have a few hurdles to cross before it can attain the near-light-speeds many experts had hoped for.

A Tale of Three Forces

According to Shen and Li’s recent research, a key problem arises once a solar light sail spacecraft begins nearing the speed of light: drag forces resulting from the very source of energy used to propel the devices could place significant limitations on their maximum attainable speeds.

A combination of different forces can be expected to occur as sunlight strikes a light sail, the authors say, which includes incident light, specular reflection, and diffuse scattering.

Incident light describes the physical momentum generated by light energy in the form of photons as they strike the sail, whereas specular reflection describes the momentum produced as photons reflect off the sail. Finally, diffuse scattering is a separate form of momentum generated by photons, which, rather than bouncing away upon impact, is actually absorbed by the sail, the energy from which is thereafter released in random directions.

New Limitations on Solar Light Sails

Based on these primary forces, the authors identify that once a light sail begins reaching relativistic speeds, it also becomes subjected to intense Doppler effect—the phenomenon that occurs as changes in the frequency of waves result as their source and an object or observer’s distance changes in relation to it.

In the case of solar light sails, the more the frequency of light waves striking the sail decreases, the less the amount of thrust generated by the three forces the paper identifies. In simpler terms, the faster a solar light sail spacecraft attempts to travel, the harder it becomes for it to accelerate.

Relativistic Light Aberration

At approximately 75% of the speed of light, the researchers say that an additional hindrance emerges, as what physicists call relativistic light aberration takes over. This phenomenon, first described by Einstein more than a century ago, involves relativistic corrections of light sources for observers who move at velocities approaching light speed.

In the case of our prospective future solar light sailors, this would mean that the weakest of the three forces impacting the sail (diffuse scattering) would begin to impose an active drag once the sail reaches approximately three-quarters of light speed. While the overall force of lasers helping to propel the light sail would remain positive at this stage in the system’s acceleration, the authors note an inevitable decline in efficiency.

The authors do concede that while their paper examines the radiative dynamics of solar light sail propulsion, it does not account for other factors that may include drag resulting from encounters with materials like gases, dust, or other physical sources (i.e., non-radiative sources), which could also impact overall speeds.

Additional factors worthy of consideration, but which the authors do not directly address in their paper, include the melting point of any materials used for solar light sail propulsion, which could be heated to extreme temperatures due to combined exposure to solar radiation, laser energy, and friction from movement.

Fundamentally, the team reports that their paper “provides a rigorous and in-depth theoretical foundation for lightsail dynamics,” which illustrates that while this future propulsion concept has its merits, we may still be far from seeing its realization for practical space travel.

By outlining the factors that contribute to constraints on light sail propulsion, Li and Shen aim to improve our overall understanding of this prospective future technology, thereby helping engineers to realize its potential for use in space exploration at some point in the future.

The team’s paper, “Relativistic Lightsail Propulsion Dynamics,” appeared on the preprint arXiv.org server.

Micah Hanks is the Editor-in-Chief and Co-Founder of The Debrief. A longtime reporter on science, defense, and technology with a focus on space and astronomy, he can be reached at micah@thedebrief.org. Follow him on X @MicahHanks, and at micahhanks.com.

It’s 2158, and you’re chugging away on your PhD in Planetary Volcanology from the University of Utopia Planitia on Mars. Graduate students still get paid a sub-living wage, so you’ve been stuck eating freeze-dried ramen for the past three years. You’ve completed studying Jupiter’s moon, Io, but now you have to leave the solar system […]

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In an ambitious collaboration bridging continents and disciplines, researchers from the University of Vienna and the Lawrence Berkeley National Laboratory have revisited one of astrophysics’ most enigmatic phenomena—the Galactic Center Excess (GCE). For over a decade, the GCE, a subtle yet pervasive gamma-ray glow enveloping the Milky Way’s core, has stimulated intense debate and exploration within the scientific community. This new study, leveraging cutting-edge machine learning methodologies, offers fresh perspectives that reinvigorate the dark matter hypothesis as a viable explanation for the GCE, a prospect previously challenged by conventional analyses.

The Galactic Center Excess presents itself as a roughly spherical halo of gamma-ray emission, extending over thousands of light years around our galaxy’s nucleus. This faint glow eludes straightforward interpretation, primarily due to the complexities of the astronomical environment it inhabits. The region is not only densely packed with astrophysical sources but also exhibits extraordinarily bright and intricately structured gamma-ray emissions, complicating efforts to disentangle the origins of the GCE signal.

Before this study, two primary interpretations vied for dominance in explaining the GCE. One posited that the excess emanates from annihilations of dark matter particles, hypothetical constituents of the universe that interact weakly with ordinary matter and light. Dark matter, while composing approximately 85% of the universe’s matter content, remains elusive, and detecting its indirect signatures through gamma-ray emissions has been a tantalizing goal. The second hypothesis attributes the gamma-ray glow to a population of millisecond pulsars—rapidly rotating neutron stars known for their intense electromagnetic emissions. These pulsars, if sufficiently numerous and faint, could collectively mimic the characteristics of the observed GCE.

However, the astrophysical scenario faced a significant analytical hurdle. Earlier statistical approaches, while sophisticated, did not fully incorporate a vital dimension of the observed data: the energy spectrum of individual gamma-ray photons. Prior analyses predominantly focused on spatial distribution patterns, searching for point sources that could represent pulsars or diffuse emissions consistent with dark matter annihilation. Without the spectral dimension, conclusions remained inconclusive, often biased toward interpretations favoring bright unresolved sources.

The breakthrough in this new research is the implementation of an advanced machine-learning framework that simultaneously evaluates the spatial location and energy distribution of gamma-ray photons captured by telescopes. Training this model required generating over a million simulated gamma-ray skies, replicating a diverse range of scenarios that include both dark matter and pulsar contributions. By synthesizing these rich datasets, the model attains unprecedented sensitivity and discrimination power, uniquely capable of parsing subtle differences in the gamma-ray energy patterns correlated with different source populations.

The enriched analysis dramatically alters the interpretation landscape. The findings demonstrate that the putative point sources—if responsible for the GCE—would need to be extraordinarily faint, to the point where their individual characteristics blur into a diffuse glow nearly indistinguishable from what dark matter annihilation models predict. This faintness requirement for pulsars implies an astronomical population count exceeding 35,000 millisecond pulsars in the central Milky Way region. Such a number challenges existing astrophysical models and contrasts with previous studies that suggested only a few hundred to a few thousand such sources would suffice to explain the gamma-ray excess.

This new quantitative insight reopens the door for dark matter as a plausible explanation. While previous evidence tended to discount dark matter in favor of point sources, the subtlety revealed by including photon energy analysis counters these assertions. It underscores the present limitations in conclusively resolving the GCE’s origin, emphasizing that the dark matter scenario remains firmly on the table alongside pulsar hypotheses.

The difficulty in resolving the GCE nature also reflects broader challenges in high-energy astrophysics—particularly in crowded celestial environments like our galaxy’s core, where overlapping emissions from stars, supernova remnants, and other celestial objects confound the interpretation of indirect dark matter signals. Machine learning, as applied here, represents a transformative tool, capable of synthesizing immense, multidimensional datasets to disentangle complex astrophysical phenomena.

Scientists caution that these findings do not constitute direct evidence for dark matter annihilation; instead, they highlight the incomplete nature of current data interpretations. The inability to definitively favor pulsars over dark matter annihilation underscores the need for next-generation gamma-ray observatories and continued advances in modeling techniques that can incorporate even more nuanced data features, such as temporal variability and polarization signatures.

This research embodies the synergy between theoretical physics, computational innovation, and observational astrophysics, demonstrating how modern data-driven approaches can revitalize longstanding scientific debates. As gamma-ray detection technologies evolve and more data become available, the methodology pioneered here promises further refinement, potentially leading to breakthroughs in identifying signals from the elusive dark sector of the universe.

The Galactic Center Excess remains one of the most compelling mysteries in contemporary astrophysics, symbolizing the frontier where known astrophysical processes intersect with profound questions about the fundamental composition of the universe. Whether future research will tilt the scales decisively in favor of dark matter or pulsars, this study exemplifies the power of interdisciplinary collaboration and sophisticated computational methods to deepen our cosmic understanding.

Moreover, the implications extend beyond academic curiosity. Deciphering the GCE carries the promise of shedding light on the nature of dark matter, a cornerstone of cosmological structure formation and evolution. Success in this endeavor could unveil new physics beyond the Standard Model, revolutionizing our conception of the universe’s fabric and the forces that govern it at the most fundamental level.

As researchers continue to probe the galactic center’s gamma-ray glow, the intellectual journey itself enriches science, reflecting a profound human drive to illuminate the obscure workings of the cosmos. This study marks a significant stride in that journey, blending technology, theory, and observation to navigate a complex astrophysical puzzle whose solution may redefine our place in the universe.

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Subject of Research: The Galactic Center Excess in gamma-ray observations and its implications for dark matter and millisecond pulsar populations.

Article Title: Energy Distribution of the Galactic Center Excess’s Sources

News Publication Date: 12-Jun-2026

Web References:
DOI link

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Keywords

Galactic Center Excess, gamma rays, Milky Way, dark matter, millisecond pulsars, machine learning, astrophysics, high-energy astrophysics, neutron stars, indirect dark matter detection, gamma-ray astronomy, astrophysical sources

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Researchers in Sweden have developed a machine-learning approach that embeds the laws of physics directly into neural networks. A new study from Chalmers University of Technology in Sweden shows that machine learning can become far more efficient when it starts with a built-in understanding of the laws of physics. Researchers found that giving an AI [...]

Bird flocks, bacterial swarms, and even crowds move according to interaction rules that appear to break one of physics’ most fundamental principles: Newton’s law of action and reaction. Birds can see much of what is happening around them, but when flying in a flock, they respond only to birds beside them or ahead of them. [...]

In a groundbreaking advancement poised to redefine core principles in theoretical physics, researchers from Kyushu University and esteemed international collaborators have unveiled insights into the nature of continuous parameters within quantum gravity. This study challenges the long-standing assumption that such parameters are freely adjustable external inputs by demonstrating—under particular theoretical conditions—that they inherently originate from operators embedded within the physical theory itself. This resolution not only revitalizes Albert Einstein’s century-old assertion regarding the intrinsic completeness of physical laws but also propels forward our comprehensive understanding of the quantum structure of spacetime.

Central to this revelation is the concept of exactly marginal operators within the framework of conformal field theory (CFT), a pivotal branch of modern physics that explores systems invariant under scale transformations. CFT serves as a formidable bridge between quantum theory and gravitational physics, especially through the lens of the anti-de Sitter/conformal field theory (AdS/CFT) correspondence. This correspondence posits a deep equivalence between gravitational theories in a curved AdS spacetime and lower-dimensional CFTs residing at its boundary, rendering CFT an indispensable tool to probe quantum gravity’s elusive traits.

At the heart of the research lies the structure known as the conformal manifold—an abstract space parameterizing a continuous family of CFTs interconnected via exactly marginal deformations. These deformations represent operators that tweak a theory’s parameters without sacrificing its conformal symmetry. The pressing theoretical puzzle was whether the existence of such a manifold necessarily implies that continuous variations in the theory’s parameters emerge from operators already encoded within the theory, rather than arbitrary, external parameters appended to the formalism.

To rigorously examine this, the interdisciplinary team led by Associate Professor Yuya Kusuki embraced an innovative approach involving conformal interfaces, mathematical constructs that serve as boundary layers interpolating between two related CFTs situated on a conformal manifold. The researchers posited that as two nearby CFTs approach equivalence, the conformal interface connecting them should become trivial. Under the plausible assumption that certain correlation functions transition smoothly as this interface dissolves, they utilized the interface’s displacement operator—which quantifies the response of the interface to infinitesimal positional shifts—to reconstruct an exactly marginal operator governing motions on the manifold.

This reconstruction represents a monumental stride because it conclusively ties continuous parameters characterizing a family of theories not to arbitrary external dials but to concrete operators intrinsic to the theory’s internal dynamics. By examining the perturbative behavior of the conformal interface, the team effectively identified the fundamental origin of parameters that might otherwise have seemed freely tunable.

What does this imply for the broader quest of quantum gravity? Through the prism of AdS/CFT duality, the intimate relationship between conformal manifolds in CFT and the moduli space of vacua in quantum gravity theories becomes transparent. This newly established principle supports the profound conjecture that quantum gravity forbids arbitrary external parameters, with all continuous couplings traceable to internal degrees of freedom—a concept resonant with a widespread expectation but hitherto unproven with such clarity.

Importantly, the present findings apply specifically to two-dimensional CFTs, a fertile domain where theoretical control is well established. Nevertheless, the researchers have expressed optimism that their methods and conceptual revelations will motivate extensions to higher-dimensional CFTs and more general quantum gravity landscapes. Extending these results could illuminate the landscape of string theories and the parameters governing candidate quantum gravity models.

Moreover, these results have significant implications for the so-called “Swampland program,” a burgeoning field striving to delineate which consistent-looking effective field theories can be embedded into quantum gravity. By constraining continuous deformations to those generated by internal operators, this study offers fresh constraints on the space of viable theories and sharpens the boundaries between the “landscape” of consistent theories and the “swampland” of inconsistent ones.

The research underscores an increasingly vital notion: the parameters defining fundamental physics are not arbitrary selections but emergent phenomena anchored within the theory’s operator framework. This insight advances a vision in which the fabric of physical law is self-contained, avoiding unexplained fundamental constants, and aligning with Einstein’s aspiration for a theory without ad hoc inputs.

Led by Kusuki alongside collaborators Shota Komatsu of CERN, Marco Meineri from the University of Turin, and Hirosi Ooguri of the California Institute of Technology, the project utilized sophisticated computational simulations combined with analytic operator algebra techniques to bring these abstract mathematical objects into clearer physical focus.

Published in the prestigious journal Physical Review Letters on June 16, 2026, the paper titled “Continuous Family of Conformal Field Theories and Exactly Marginal Operators” delineates these technical breakthroughs and their broader theoretical implications, offering a compelling blueprint for future explorations in the intersection of quantum theory and gravity.

As the physics community absorbs the ramifications of this breakthrough, it heralds a renewed momentum for using conformal field theory and holographic dualities as guiding principles to unravel the enigmatic quantum nature of gravitation, spacetime, and the universe’s foundational constants.

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Subject of Research: Not applicable

Article Title: Continuous Family of Conformal Field Theories and Exactly Marginal Operators

News Publication Date: 16-Jun-2026

Web References: Kyushu University Institute for Advanced Study, Kyushu University

References: Shota Komatsu, Yuya Kusuki, Marco Meineri, and Hirosi Ooguri, Physical Review Letters, 16 June 2026.

Image Credits: Yuya Kusuki/Kyushu University

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Keywords

Quantum Gravity, Conformal Field Theory, Exactly Marginal Operators, Conformal Manifold, Quantum Moduli Space, AdS/CFT Correspondence, Operator Reconstruction, Displacement Operator, Conformal Interface, Fundamental Constants, Theoretical Physics, Swampland Conjecture