Why stars spin down, or up, before they die

Illustration of the inner regions of a massive star during its final oxygen (green) and silicon (teal) shell burning phase, before the collapse of the iron core (indigo). The strength and geometry of the magnetic field, combined with the properties of convection in the oxygen region can cause the rotation rate to speed up or slow down.
Image Credit: KyotoU / Lucy McNeill

Scientific Frontline: Extended "At a Glance" Summary: Stellar Rotational Evolution and Magnetic Fields

The Core Concept: The rotation rate of massive stars evolves dynamically over their lifetimes, driven by the complex interaction between violent convection, rotation, and magnetic fields within their interiors. Recent 3D magnetohydrodynamic simulations demonstrate that while most stars spin down as they age, specific magnetic configurations in the convection zone can actually transport angular momentum inward, causing the stellar core to spin up before death.

Key Distinction/Mechanism: Previous models primarily attributed stellar "spin-down" to the gradual shedding of mass and angular momentum via stellar winds (like the solar wind). This new mechanism demonstrates that internal magnetic field geometry directly controls the radial transport of angular momentum during advanced burning phases, revealing that final spin rates are heavily dependent on internal magnetic properties rather than mass loss alone.

Major Frameworks/Components: 

• Asteroseismology: An observational technique that measures a star's natural oscillation frequencies to ascertain internal rotation rates and magnetic field strengths.
• 3D Magnetohydrodynamic (MHD) Simulations: Advanced computational models utilized to observe massive stars just before core-collapse, analyzing the interplay of fluid dynamics and magnetism.
• Solar Dynamo Analogy: The theoretical framework suggesting that the coevolution of internal rotation and magnetic fields in massive stars functions similarly to the energy processes sustaining the Sun's magnetic field.
• Radial Transport of Angular Momentum: A formulated model describing how energy and momentum move outward or inward during late-stage burning phases (e.g., oxygen and silicon shell burning), dictated by magnetic field geometry.

How solar prominences form

The new computer simulations are based on a magnetic field structure that is often associated with prominences: the magnetic field lines in the corona form a double arc with a small dip in the middle. As the calculations show, the flame-like prominence forms in this dip and remains trapped there. All relevant layers of the Sun were taken into account, from the corona, the Sun’s outer atmosphere, to parts of the convection zone below the Sun’s surface.
Image Credit: © MPS

Scientific Frontline: Extended "At a Glance" Summary: Solar Prominence Supply Mechanisms

The Core Concept: Solar prominences are massive, densely packed structures of relatively cool plasma that extend for thousands of kilometers into the Sun's exceptionally hot outer atmosphere, the corona.

Key Distinction/Mechanism: Unlike the surrounding corona, which burns at over one million degrees, prominences consist of plasma cooled to approximately 10,000 degrees. They remain suspended and stable for weeks due to a delicate supply balance: turbulent magnetic forces in the cooler, lower layer of the Sun (the chromosphere) eject bursts of cool plasma upward, while hot coronal plasma simultaneously flows into magnetic dips and condenses, offsetting material that "rains" back down.

Major Frameworks/Components:

• Double-Arc Magnetic Architecture: Magnetic field lines in the corona frequently form a double arch resembling two adjacent mountains; the cool prominence material forms and becomes trapped within the central dip.
• Chromospheric Injection: Turbulent, small-scale magnetic field movements beneath the corona forcefully eject cool plasma upward to feed the prominence.
• Coronal Condensation: Secondary supply logistics occur when hot plasma travels along magnetic field lines into the central dip, where it cools and condenses.
• Multi-Layered Simulation Models: The research framework accounts for all relevant solar layers concurrently, linking turbulent plasma flows below the visible surface, the cooler chromosphere, and the extremely hot corona.

The Local Universe’s Expansion Rate Is Clearer Than Ever, but Still Doesn’t Add Up

Artist’s interpretation of the cosmic distance ladder — a succession of overlapping methods used to measure distances across the Universe, where each rung of the ladder provides information that can be used to determine the distances at the next higher rung. Methods include observations of pulsating Cepheid variable stars, red giant stars that shine with a known brightness, Type Ia supernovae, and certain types of galaxies.  In this illustration, the distance ladder begins at the Coma Cluster, which is the nearest extremely rich galaxy cluster to us. The distance to the Coma Cluster can be measured directly using observations of Type Ia supernovae within the cluster. Type Ia supernovae have a predictable luminosity that makes them reliable objects for distance calculations. 
Image Credit: CTIO/NOIRLab/DOE/NSF/AURA/J. Pollard

Scientific Frontline: Extended "At a Glance" Summary: The Hubble Tension and the Local Distance Network

The Core Concept: The Hubble tension is a persistent, statistically significant discrepancy between the Universe's expansion rate measured in the local Universe and the rate predicted from the early Universe using the standard model of cosmology.

Key Distinction/Mechanism: Rather than relying on a single measurement method, this breakthrough framework unites decades of independent distance measurements into a unified "distance network." By cross-linking overlapping techniques—such as observing Cepheid variable stars, red giant stars, and Type Ia supernovae—astronomers achieved a local expansion rate of 73.50 ± 0.81 km/s/Mpc with roughly 1% precision. This multi-path approach effectively rules out single-method observational errors as the cause of the discrepancy with the early Universe prediction of 67–68 km/s/Mpc.

Major Frameworks/Components: 

• The Standard Model of Cosmology: The theoretical baseline used to predict the present-day expansion rate based on cosmic microwave background measurements.
• The Cosmic Distance Ladder/Network: An observational methodology utilizing multiple independent, overlapping distance indicators to measure the local Universe.
• H0 Distance Network (H0DN) Collaboration: An international, community-built framework synthesizing independent astrophysical measurements from both ground and space-based observatories, including the NSF NOIRLab programs.

A Solar System in the making? Two planets spotted forming in disc around young star

This image shows two planets being born around the young star WISPIT 2. These observations were made with the SPHERE instrument at ESO’s Very Large Telescope (VLT). SPHERE can directly image exoplanets by correcting atmospheric turbulence and blocking the light from the central star.   This composite image contains SPHERE observations carried out at different epochs. The outermost planet, WISPIT 2b, was discovered first, whereas WISPIT 2c, which orbits much closer to the star, was confirmed afterwards. 
Image Credit: ESO/C. Lawlor, R. F. van Capelleveen et al.

Scientific Frontline: "At a Glance" Summary: WISPIT 2 Planetary System

• Main Discovery: Astronomers confirmed the presence of a second developing gas giant, WISPIT 2c, within the planet-forming disk of the young star WISPIT 2, establishing it as only the second known system where multiple forming planets have been directly observed.
• Methodology: Researchers captured direct images of the object using the SPHERE instrument on the European Southern Observatory's Very Large Telescope and confirmed its planetary status utilizing the recently upgraded GRAVITY+ instrument on the VLT Interferometer.
• Key Data: WISPIT 2c is roughly ten times the mass of Jupiter and orbits four times closer to the central star than the previously discovered WISPIT 2b, which possesses five times Jupiter's mass and an orbit sixty times the distance between the Earth and the Sun.
• Significance: The system features an extended disk with distinct dust rings and gaps carved by accumulating planetary embryos, providing a critical observational laboratory for studying how young planetary systems evolve into mature configurations akin to our own Solar System.
• Future Application: Astronomers plan to utilize the upcoming Extremely Large Telescope to conduct follow-up observations and attempt direct imaging of a suspected third, Saturn-mass planet that may be carving a narrower, shallower outer gap in the disk.
• Branch of Science: Astronomy, Astrophysics, Planetary Science

New Explanation for Unique ‘Negative Superhump’ Features of Deep-Space Binary Star Systems

Image Credit: S. Lepp (UNLV) / AI illustration

Scientific Frontline: "At a Glance" Summary: Negative Superhump Features in Deep-Space Binary Star Systems

• Main Discovery: Astrophysicists have proposed a new theoretical model explaining negative superhumps in cataclysmic variable star systems, determining that these periodic brightness variations are caused by an elongated, eccentric accretion disk rather than a tilted circular disk.
• Methodology: Researchers developed a framework demonstrating that an eccentric accretion disk gradually rotates its orbit backwards over time through pressure-driven retrograde apsidal precession, naturally producing negative superhumps without requiring a physical disk tilt.
• Key Data: The eccentric disk model accounts for the prevalence of negative superhumps across a wide range of binary star masses and explains conditions where both positive and negative superhumps can temporarily coexist, resolving observational anomalies dating back to the 1970s.
• Significance: This theoretical advancement resolves a decades-old astronomical conundrum by eliminating the unproven requirement of a tilted accretion disk, providing a more physically sound explanation for the mechanisms driving the evolution of binary star systems.
• Future Application: Scientists will utilize large-scale numerical simulations to model evolving accretion disks, aiming to match predicted light curves with observational data and investigate the formation of positive superhumps in high mass ratio systems.
• Branch of Science: Astrophysics and Astronomy.

'Space Archaeology' Reveals First Dynamic History of a Giant Spiral Galaxy

An artist's impression shows the giant spiral galaxy NGC 1365 as it collides and merges with a smaller companion galaxy, stirring up star formation and redistributing gas and heavy elements. Using a new "space archaeology" technique that reads the chemical fingerprints in the galaxy’s gas, astronomers have reconstructed how NGC 1365 grew over 12 billion years.
Image Credit: Melissa Weiss/CfA

Scientific Frontline: Extended "At a Glance" Summary: Extragalactic Archaeology and the Evolution of NGC 1365

The Core Concept: Extragalactic archaeology is a novel astronomical technique that reconstructs the multi-billion-year evolutionary history of distant galaxies by analyzing the detailed chemical fingerprints embedded in their gas and star-forming clouds.

Key Distinction/Mechanism: Unlike traditional observations that capture a static snapshot of a galaxy, this method maps the distribution of heavy elements (such as oxygen) across a galaxy's structure using high-resolution spectroscopy. These chemical patterns are then compared against state-of-the-art cosmological simulations to infer the galaxy's historical timeline, including past mergers, gas flows, and star formation rates over cosmic time.

Major Frameworks/Components:

• TYPHOON Survey: An observational initiative utilizing the Irénée du Pont telescope to achieve sharp resolutions of individual star-forming clouds, isolating specific diagnostic emission lines (like ionized hydrogen, nitrogen, and oxygen) across the galaxy's disk.
• Chemical Fingerprinting: The process of analyzing the light emitted by excited gases around young, hot stars to measure the concentration and distribution of heavy elements from the galactic center to the outer spiral arms.
• The Illustris Project: Advanced cosmological simulations that model the physical processes of the universe—such as gas motion, black hole activity, and chemical evolution—used to find a precise theoretical match to the observed data.

Stars like our Sun may maintain the same rotation pattern for life, contrary to 45 years of theoretical predictions

Solar magnetic activity observed by NASA’s Solar Dynamics Observatory spacecraft.
Image Credit: NASA/SDO and the AIA, EVE, and HMI science teams.

Scientific Frontline: "At a Glance" Summary: Solar-Type Star Rotation Patterns

• Main Discovery: Stars similar to our Sun maintain a solar-type differential rotation throughout their entire lifetime—spinning faster at the equator than at the poles—disproving a 45-year-old theory that older, slower-rotating stars eventually switch their rotation patterns.
• Methodology: Researchers from Nagoya University conducted extremely high-resolution simulations of the interior of solar-type stars using Japan's Fugaku supercomputer, dividing each simulated star into 5.4 billion grid points to track gas flows and magnetic activity.
• Key Data: The simulations processed 5.4 billion grid points per star to accurately reflect that a star's equator completes a rotation in approximately 25 days compared to 35 days for the poles, a differential pattern sustained across its lifespan.
• Significance: The unprecedented resolution of the simulations revealed that internal magnetic fields stay robust enough to prevent a rotation flip, effectively correcting decades of low-resolution theoretical models where magnetic fields artificially disappeared and produced inaccurate predictions.
• Future Application: This corrected stellar interior model will help scientists solve lingering mysteries such as the Sun's 11-year sunspot cycle, refine star evolution models, and better predict how long-term magnetic activity affects the habitability of surrounding exoplanets.
• Branch of Science: Astronomy and Astrophysics.
• Additional Detail: The new simulations also established that the magnetic fields of stars weaken continuously throughout their lives, contradicting previous assumptions that magnetic fields would strengthen again during old age.

Hydrogen sulfide detected in distant gas giant exoplanets for the first time

This animation shows the four giant planets orbiting HR 8799, located 133 light-years from Earth. The movie combines real images captured at the W.M. Keck Observatory between 2009 and 2021, with the planets’ orbital motion smoothed by modeling their orbital paths around the star.
Image Credit: W. Thompson (NRC-HAA), C. Marois (NRC-HAA), Q. Konopacky (UCSD) 

Scientific Frontline: "At a Glance" Summary

• Main Discovery: Astronomers detected hydrogen sulfide molecules for the first time in the atmospheres of four massive gas giant exoplanets orbiting the star HR 8799.
• Methodology: Researchers utilized spectral data from the James Webb Space Telescope (JWST), applying new data analysis algorithms to suppress starlight and creating specialized atmospheric models to identify the unique light absorption signatures of sulfur.
• Key Data: The target system is located 133 light-years away in the constellation Pegasus, with the observed planets ranging from 5 to 10 times the mass of Jupiter and orbiting at distances greater than 15 astronomical units from their host star.
• Significance: The presence of sulfur indicates these bodies formed by accreting solid particles from a protoplanetary disk rather than collapsing directly from gas, definitively classifying them as planets rather than brown dwarfs.
• Future Application: The signal processing techniques developed for this study establish a viable method for characterizing the atmospheres of smaller, rocky worlds and searching for biosignatures on Earth-like exoplanets in the future.
• Branch of Science: Astronomy, Astrophysics and Planetary Science.
• Additional Detail: The study reveals that these distant giants share a heavy element enrichment pattern similar to Jupiter and Saturn, suggesting a universal formation mechanism for gas giants across different stellar systems.

What Is: Cosmic Event Horizon

The Final Boundary
An illustration of the Cosmic Event Horizon. Unlike the Observable Universe, which is defined by light that has reached us, this horizon marks the limit of causal contact. Beyond this line, space expands faster than the speed of light, meaning no signal sent from Earth today could ever overtake the expansion to reach galaxies in these regions.
Image Credit: Scientific Frontline

Scientific Frontline: Extended "At a Glance" Summary

• The Core Concept: A theoretical boundary in the universe separating events that can ever causally affect an observer from those that never will; effectively, it marks the absolute limit of future visibility.
• Key Distinction/Mechanism: Unlike the Particle Horizon (which defines the observable past) or the Hubble Sphere (a kinematic boundary where recession velocity equals the speed of light), the Event Horizon is a strict causal limit determined by the accelerating expansion of space. Light emitted from galaxies beyond this horizon at the present moment will never reach Earth, regardless of how much time passes.
• Origin/History: Rooted in the standard \(\Lambda\)CDM model of cosmology; current interest is driven by the "Crisis in Cosmology" regarding Dark Energy and the Cosmological Coupling hypothesis, which suggests a link between black hole growth and cosmic expansion.
• Major Frameworks/Components:
• \(\Lambda\)CDM Model: The standard framework involving Dark Energy and Cold Dark Matter that predicts the horizon's existence.
• FLRW Metric: The geometry of spacetime describing an expanding universe.
• Cosmological Coupling: A recent hypothesis positing that black holes are the source of Dark Energy.
• Black Hole Cosmology: A theoretical model suggesting our observable universe may be the interior of a black hole within a larger parent universe.
• Branch of Science: Cosmology, Astrophysics, Theoretical Physics.
• Future Application: Critical for refining models of Dark Energy and testing the limits of General Relativity; ultimately essential for predicting the long-term fate of the universe (e.g., "Cosmic Solitude").
• Why It Matters: It defines the fundamental limits of our reality and causal connection to the rest of the cosmos. Recent theories connecting this horizon to black hole physics could radically alter our understanding of the Big Bang, suggesting our universe is a "cell" within a larger multiverse rather than an isolated expanse.

UrFU Researchers Discovered “Laughing Gas” in Interstellar Ices around Protostars

Anton Vasyunin leads the research group and laboratory.
Photo Credit: UrFU press service

Scientific Frontline: Extended "At a Glance" Summary

The Core Concept: Researchers have definitively identified nitrous oxide (N₂O), commonly known as "laughing gas," within the solid ice mantles coating dust particles around young protostars.

Key Distinction/Mechanism: Unlike the gas phase of the interstellar medium—where over 300 molecules have been identified—molecules in the solid "ice" phase are notoriously difficult to detect and are only visible via infrared absorption spectra. N₂O is only the ninth molecule ever confirmed in this frozen state.

Origin/History:

• January 2026: Findings were reported by the Ural Federal University (UrFU) and published in the journal Astronomy and Astrophysics.
• Methodology: The discovery relied on observational data from the James Webb Space Telescope (JWST), which was interpreted using laboratory-generated spectra of ice analogues created at UrFU's ISEAge laboratory.

Major Frameworks/Components:

• Infrared Spectroscopy: The primary method used to detect molecular signatures in solid ices, requiring background starlight to "illuminate" the absorption features.
• Protostars: The study analyzed 50 young stars, finding N₂O in 16 of them.
• Orion Molecular Cloud: A specific region where half of the positive detections were located, suggesting that high-intensity ultraviolet radiation aids in N₂O formation.

Branch of Science: Astrochemistry, Astrophysics.

Future Application: These findings improve models of chemical evolution in the universe, helping scientists understand how complex volatiles form and survive in the raw materials that eventually coalesce into planetary systems.

Why It Matters: This discovery indicates that nitrous oxide is relatively abundant in star-forming regions (found in nearly a third of surveyed targets), adding a critical piece to the puzzle of how prebiotic chemistry develops in the freezing vacuum of space before planets are born.

International astronomical survey captures remarkable images of the “teenage years” of new worlds

This ARKS gallery of faint debris disks reveals details about their shape: belts with multiple rings, wide smooth halos, sharp edges, and unexpected arcs and clumps, which hint at the presence of planets shaping these disks; and chemical make-up: the amber colors highlight the location and abundance of the dust in the 24 disks surveyed, while the blue their carbon monoxide gas location and abundance in the six gas-rich disks.
Image Credit: Sebastian Marino, Sorcha Mac Manamon, and the ARKS collaboration

Scientific Frontline: Extended "At a Glance" Summary

The Core Concept: The ARKS (ALMA survey to Resolve exoKuiper belt Substructures) program is an international astronomical survey that has captured the first high-resolution images of debris disks, which represent the chaotic "teenage" phase of planetary system evolution.

Key Distinction/Mechanism: Unlike the bright, gas-rich disks of newborn planets ("baby pictures"), these "teenage" systems are fainter dusty belts that exist after planets have formed but before the system settles into adulthood; the survey utilizes the Atacama Large Millimeter/submillimeter Array (ALMA) to resolve minute details like dust grains and carbon monoxide gas, revealing complex substructures rather than simple, uniform rings.

Origin/History: The survey team, led by the University of Exeter, secured approximately 300 hours of observation time at the ALMA observatory between October 2022 and July 2024, with findings published in a series of papers in Astronomy & Astrophysics.

Cosmic Lens Reveals Hyperactive Cradle of Future Galaxy Cluster

The galaxy cluster lens J0846 in optical light (bottom right), the ALMA view of dust-enshrouded, star-forming galaxies strongly lensed into bright arcs (top right), and a composite view (left) revealing at least 11 dusty galaxies in a compact protocluster core more than 11 billion light-years away, magnified by the foreground cluster’s gravity.
Image Credit: NSF/AUI/NSF NRAO/B. Saxton; NSF/NOIRLab

Galaxy clusters are formed by a dense packing of many galaxies, making them the most massive structures in the Universe. Their progenitors, protoclusters, show these galaxies in their infancy, offering a window to study how they all formed. This early “settlement” of galaxies will eventually evolve into a sprawling metropolis by the present day. Astronomers using the U.S. National Science Foundation Very Large Array (NSF VLA) and the Atacama Large Millimeter/submillimeter Array (ALMA) have discovered a rare protocluster that was exceptionally bright, all when the Universe was 11 billion years younger. The system, called PJ0846+15 (J0846), is the first strongly lensed protocluster core discovered, revealing how some of the most massive galaxy clusters in the present-day Universe began their lives.

Young Galaxies Grow Up Fast

The 18 galaxies from the ALPINE-CRISTAL-JWST survey. Each picture shows the location of ionized gas (as traced by the hydrogen alpha line, the spectral signature of hot hydrogen gas) in the galaxies. Several of the pictured galaxies are interacting, meaning two or even three galaxies are in the process of merging.
Image Credit: Andreas Faisst (Caltech) and the ALPINE-CRISTAL-JWST Survey team

Astronomers have captured the most detailed look yet at faraway galaxies at the peak of their youth, an active time when the adolescent galaxies were fervently producing new stars. The observations focused on 18 galaxies located 12.5 billion light-years away. They were imaged across a range of wavelengths from ultraviolet to radio over the past eight years by a trio of telescopes: NASA's Hubble Space Telescope; NASA's James Webb Space Telescope (JWST); and ALMA (Atacama Large Millimeter/submillimeter Array) in Chile, of which the U.S. National Science Foundation National Radio Astronomy Observatory is a partner. Data from other ground-based telescopes were also used to make measurements, such as the total mass of stars in the galaxies.

"With this sample, we are uniquely poised to study galaxy evolution during a key epoch in the universe that has been hard to image until now," says Andreas Faisst, a staff scientist at IPAC, a science and data center for astronomy at Caltech. "Thanks to these exceptional telescopes, we have spatially resolved these galaxies and can observe the stages of star formation as they were happening and their chemical properties when our universe was less than a billion years old."

Earliest, hottest galaxy cluster gas on record could change our cosmological models

Artist’s impression of a forming galaxy cluster in the early universe: radio jets from active galaxies are embedded in a hot intracluster atmosphere (red), illustrating a large thermal reservoir of gas in the nascent cluster.
Image Credit: Lingxiao Yuan

The scorching cloud of gas threaded between clusters of galaxies is five times hotter than current models predict, highlighting gaps in our models of galaxy cluster formation.

An international team of astronomers led by Canadian researchers has found something the universe wasn’t supposed to have: a galaxy cluster blazing with hot gas just 1.4 billion years after the Big Bang, far earlier and hotter than theory predicts.  

The result, published in Nature, could upend current models of galaxy cluster formation, which predict such temperatures will occur only in more mature, stable galaxy clusters later in the universe’s life.  

“We didn’t expect to see such a hot cluster atmosphere so early in cosmic history,” said lead author Dazhi Zhou, a PhD candidate in the UBC department of physics and astronomy. “In fact, at first, I was skeptical about the signal as it was too strong to be real. But after months of verification, we’ve confirmed this gas is at least five times hotter than predicted, and even hotter and more energetic than what we find in many present-day clusters.”  

A speed camera for the universe

The stars (or rather galaxies) of the show.
A montage of eight time-delay gravitational lens systems. There’s an entire galaxy at the center of each image, and the bright points in rings around them are gravitationally lensed images of quasars behind the galaxy. These images are false-color and are composites of data from different telescopes and instruments.
Image Credit: ©2025 TDCOSMO Collaboration et al.
(CC BY-ND 4.0)

There is an important and unresolved tension in cosmology regarding the rate at which the universe is expanding, and resolving this could reveal new physics. Astronomers constantly seek new ways to measure this expansion in case there may be unknown errors in data from conventional markers such as supernovae. Recently, researchers including those from the University of Tokyo measured the expansion of the universe using novel techniques and new data from the latest telescopes. Their method exploits the way light from extremely distant objects takes multiple pathways to get to us. Differences in these pathways help improve models on what happens at the largest cosmological scales, including expansion.

Helium leak on the exoplanet WASP-107b

Artist's view of WASP-107b. The planet’s low density and the intense irradiation from its star allow helium to escape the planet and form an asymmetric extended and diffuse envelope around it.
Image Credit: © University of Geneva/NCCR PlanetS/Thibaut Roger

An international team including UNIGE observed with the JWST huge clouds of helium escaping from the exoplanet Wasp-107b. 

An international team, including astronomers from the University of Geneva (UNIGE) and the National Centre of Competence in Research PlanetS, has observed giant clouds of helium escaping from the exoplanet WASP-107b. Obtained with the James Webb Space Telescope, these observations were modeled using tools developed at UNIGE. Their analysis, published in the journal Nature Astronomy, provides valuable clues for understanding this atmospheric escape phenomenon, which influences the evolution of exoplanets and shapes some of their characteristics. 

Sometimes a planet’s atmosphere escapes into space. This is the case for Earth, which irreversibly loses a little over 3 kg of matter (mainly hydrogen) every second. This process, called ‘‘atmospheric escape’’, is of particular interest to astronomers for the study of exoplanets located very close to their star, which, heated to extreme temperatures, are precisely subject to this phenomenon. It plays a major role in their evolution. 

Stars defy the black hole: research in Cologne shows stable orbits around Sagittarius A*

Image Credit: NASA

New observations made with the ERIS instrument at the Very Large Telescope facility disprove from the assumption that the supermassive black hole at the center of the Milky Way devours nearby dust objects. 

An international research team led by PD Dr Florian Peißker at the University of Cologne has used the new observation instrument ERIS (Enhanced Resolution Imager and Spectrograph) at the Very Large Telescope (VLT) facility in Chile to show that several so-called ‘dusty objects’ follow stable orbits around the supermassive black hole Sagittarius A* at the center of our galaxy. Earlier studies had surmised that some of these objects could be swallowed up by the black hole. New data refutes this assumption. The findings have been published under the title ‘ABCD’ in the journal Astronomy & Astrophysics. 

The study focused on four of these unusual celestial bodies, which have been the subject of much discussion in recent years. In particular, G2 was long regarded as a pure dust and gas cloud. It was thought to have been initially elongated by the gravitational pull of Sagittarius A*, a process known as 'spaghettification', before being destroyed. However, the specific observations made with ERIS, which captures radiation in the near-infrared range, show that G2 follows a stable orbit. This is an indication that there is a star inside the dust cloud. These results confirm that the center of the Milky Way is not only destructive but can also be surprisingly stable. 

A sparkling ‘Diamond Ring’ in space: Astronomers in Cologne unravel the mystery of a cosmic ring

Stars Brewing in Cygnus X
Image Credit: NASA/JPL-Caltech/Harvard-Smithsonian CfA

The structure of gas and dust resembles a glowing diamond ring. Computer simulations and observations made on board the 'flying observatory' SOFIA are now able to explain the special shape. 

An international team led by researchers from the University of Cologne has solved the mystery of an extraordinary phenomenon known as the ‘Diamond Ring’ in the star-forming region Cygnus X, a huge, ring-shaped structure made of gas and dust that resembles a glowing diamond ring. In similar structures, the formations are not flat but spherical in shape. How this special shape came about was previously unknown. The results have been published under the title ‘The Diamond Ring in Cygnus X: an advanced stage of an expanding bubble of ionized carbon’ in the journal Astronomy & Astrophysics. 

The ring has a diameter of around 20 light years and shines strongly infrared light. It is the relic of a former cosmic bubble that was once formed by the radiation and winds of a massive star. In contrast to other similar objects, the ‘Diamond Ring’ does not have a rapidly expanding spherical shell, but only a slowly expanding ring. 

Astronomers discover a superheated star factory in the early universe

Glowing deep red from the distant past: galaxy Y1 shines thanks to dust grains heated by newly-formed stars (circled in this image from the James Webb telescope).
Image Credit: NASA, ESA, CSA, STScI, J. Diego (Instituto de Física de Cantabria, Spain), J. D’Silva (U. Western Australia), A. Koekemoer (STScI), J. Summers & R. Windhorst (ASU), and H. Yan (U. Missouri)

Astronomers have uncovered a previously unknown, extreme kind of star factory by taking the temperature of a distant galaxy using the ALMA telescope. The galaxy is glowing intensely in superheated cosmic dust while forming stars 180 times faster than our own Milky Way. The discovery indicates how galaxies could have grown quickly when the universe was very young, solving a long-standing puzzle for astronomers.  

The first generations of stars formed under conditions very different from anywhere we can see in the nearby universe today. Astronomers are studying these differences using powerful telescopes that can detect galaxies so far away their light has travelled towards us for billions of years.   

Astronomy: In-Depth Description

James Webb Space Telescope view of IRAS 04302+2247, a planet-forming disc located about 525 light-years away in a dark cloud within the Taurus star-forming region.
Image Credit: ESA/Webb, NASA & CSA, M. Villenave et al.

Astronomy is the natural science dedicated to the study of all celestial objects and phenomena originating beyond Earth's atmosphere. Its primary goals are to understand the physical and chemical properties of these objects, their origins and evolution, and the fundamental laws governing the universe as a whole.