Stunning Close-Ups of Triangular Galaxies Captured by ESO’s Very Large Telescope (VLT) Illuminate the Gas and Dust That Fuel Star Birth and Galaxy Evolution.
This VLT/MUSE image showcases the Triangulum Galaxy, a spiral galaxy approximately 3 million light-years away in the constellation Triangulum. Image credit: ESO / Feltre et al.
The Triangulum Galaxy, also referred to as Messier 33 or NGC 598, is a spiral galaxy located roughly 3 million light-years from Earth.
Visible as a faint haze in the Triangulum constellation under optimal dark sky conditions, this galaxy has long captivated astronomers.
It stands as one of the most significant members of the Local Group, a gravitationally bound assembly of over 50 galaxies, including the Milky Way and Andromeda. Though third largest in the group, it is the smallest spiral galaxy in this collection.
Spanning about 60,000 light-years, the Triangulum Galaxy is substantially smaller than Andromeda, which measures around 200,000 light-years, and the Milky Way, estimated at 100,000 light-years in diameter.
Dr. Anna Feltre and her colleagues from the INAF Astrophysical Observatory in Arcetri emphasized, “Stars do not exist in isolation; they thrive in rich, complex environments where they actively form.”
“Investigating these cosmic interactions enhances our understanding of star formation and the influence of their radiation on surrounding matter, which is crucial for unraveling how galaxies evolve,” they added.
In their research, astronomers utilized data collected by the VLT’s Multi-Unit Spectroscopic Explorer (MUSE).
“MUSE’s unique capability allows it to disperse light into a spectrum of colors, enabling us to analyze the chemical makeup of the interstellar medium across the entire field,” the team elaborated.
The vivid colors in the images signify various elements: blue, green, and red represent oxygen, hydrogen, and sulfur, respectively.
“Thanks to MUSE, we have mapped the distribution and motion of numerous elements, crucial for understanding the connections between stars and their environments.”
“These cosmic interactions create a visually stunning and dynamic landscape, revealing that star birthplaces are more intricate and beautiful than we ever envisioned,” concluded Dr. Feltre.
For in-depth insights, refer to the team’s paper published in the journal Astronomy and Astrophysics.
_____
A. Feltre et al. 2026. M3D: Mosaicking M33 using the MUSE datacube. I. Elucidating the Diversity of the H II Region of M33 Using MUSE. A&A 706, A367; doi: 10.1051/0004-6361/202557122
The newly discovered gas cloud, known as G2t, shares an almost identical orbit with two previously identified clouds, indicating that they may have originated from a pair of massive stars situated near the Milky Way’s core.
This VLT image illustrates the stars and gas surrounding Sagittarius A*, the supermassive black hole at the center of the Milky Way. Image credit: ESO/D. Ribeiro, MPE GC Team.
“This is a dynamic environment where stars and gas clouds orbiting the black hole move at astonishing speeds,” remarked Dr. Stefan Gillessen from the Max Planck Institute for Extraterrestrial Physics.
“While the gas clouds G1 and G2 were previously known, their origins and compositions remained subjects of debate.”
“Specifically, questions arose about whether these clouds contained hidden stars or were purely gaseous.”
“With the identification of G2t, we are starting to unravel these mysteries.”
G2t was detected using the High-Resolution Imager and Spectrograph (ERIS) on the ESO’s Very Large Telescope (VLT).
“Thanks to the VLT, we successfully measured the 3D orbit of this gas cloud around the black hole,” the team explained.
“G2t traverses a remarkably small area within this expansive image of the center.”
“Interestingly, G1, G2, and G2t are found to have nearly identical orbits, albeit slightly tilted in relation to one another.”
“The odds of different stars maintaining such similar orbits are minimal, further suggesting that each cloud does not harbor a star at its core.”
“These orbital similarities indicate that all three clouds likely stem from the same source, most probably IRS16SW, a pair of massive stars that discharge substantial quantities of gas.”
“As IRS16SW moves around the black hole, each gas cloud is ejected on a slightly different trajectory, explaining the subtle variations observed among the ‘G-triplets.’
“This finding highlights that despite years of observing our galaxy’s center, fresh enigmas await discovery,” the researchers noted.
“What could be more thrilling than a mystery poised to be unraveled?”
For more about this discovery, refer to the paper published in the journal Astronomy and Astrophysics.
_____
S. Gillessen et al. 2026. Gas streamer G1-2-3 at the center of the galaxy. A&A 707, A79; doi: 10.1051/0004-6361/202555808
Tomassini et al. characterized the physical and morphological properties of AFGL 4106, a binary star system of two evolved massive stars. Image credit: ESO / Tomassini et al..
“Before a star reaches the end of its life cycle, it expels massive amounts of gas and dust that contribute to the formation of a growing nebula,” stated Dr. Gabriel Tomassini from the Côte d’Azur Observatory and colleagues.
“The massive stars in the AFGL 4106 system are in advanced but distinct stages of their lifecycle, with one having shed enough mass to form a surrounding dusty envelope.”
In their recent study, the authors meticulously map this cosmic debris to identify the characteristics of AFGL 4106’s central star.
“Imaging objects near a bright star presents significant challenges due to the star’s overwhelming brightness. In fact, the central star appears black as its brilliance saturates the image detectors,” noted the researchers.
“Fortunately, the VLT’s SPHERE instrument excels at managing significant light contrasts, enabling detailed observation of both the luminous stars and their darker surrounding nebulae for the first time.”
“It also corrects for atmospheric turbulence, providing remarkably clear images.”
The nebula’s unique shape indicates that the companion star significantly affects the gas outflow from the dying star, introducing asymmetry and distorting the gas and dust cloud from a perfectly spherical shape.
“Our findings place constraints on the physical properties and evolutionary status of the system,” concluded the astronomers.
“This research enhances our understanding of mass loss processes in massive binary stars and the morphology of nebulae surrounding evolved stars.”
Results from this study are detailed in the journal Astronomy and Astrophysics.
_____
G. Tomassini et al.. 2026. Characterizing the post-red supergiant binary system AFGL 4106 and its complex nebula with SPHERE/VLT. A&A 706, A5; doi: 10.1051/0004-6361/202557705
A global team of astronomers from Chile, Europe, the USA, Canada, and New Zealand has achieved an unprecedented level of detail in spectroscopic observations of an interstellar comet as it moves through our solar system. Utilizing spectroscopic data from two instruments on the ESO’s Very Large Telescope (VLT), researchers detected emissions of nickel atoms and cyan gas from the interstellar comet 3I/ATLAS, marking it as the third confirmed interstellar object recorded.
This image of interstellar comet 3I/ATLAS was taken with Hubble’s Wide Field Camera 3 (WFC3) on December 27, 2025. Image credit: NASA/ESA/CSA/Hubble.
The interstellar traveler, 3I/ATLAS, was first discovered on July 1, 2025, using the NASA-funded ATLAS (Asteroid Terrestrial Impact Last Alert System) telescope.
Also referred to as C/2025 N1 (ATLAS) and A11pl3Z, this celestial object approached from the constellation Sagittarius.
At its discovery, the comet was located 4.51 astronomical units (AU) from the Sun, with an eccentricity of 6.13.
“Understanding the volatile components of interstellar objects that pass through our solar system grants us unique insights into the chemical and physical processes occurring in distant stellar systems,” noted Dr. Rohan Rahatgaonkar of the Catholic University of Chile.
“Interstellar objects maintain remnants of the chemical and physical processes active in their protoplanetary disks during formation and may be altered by interstellar medium exposure.”
“When subjected to solar radiation, these cometary interstellar objects emit solids and gases due to their activity.”
During July and August, astronomers carried out high-resolution spectroscopic analyses as 3I/ATLAS approached between 4.4 to 2.85 AU from the Sun.
To acquire the comet’s spectrum, they employed the VLT’s X-Shooter and the Ultraviolet and Visible Echelle Spectrometer (UVES).
Observations revealed that the comet’s coma, the cloud of dust and gas enveloping its nucleus, is primarily made up of dust, with a consistent reddish optical continuum indicating organic-rich materials.
This reddish coloration resembles that of comets within our solar system and primitive Kuiper belt objects, suggesting shared physical processes across the planetary system.
3I/ATLAS spectrum showing Ni I emission over observations from VLT/X-Shooter and VLT/UVES. Image credit: Rahatgaonkar et al., doi: 10.3847/2041-8213/ae1cbc.
As 3I/ATLAS continued its journey towards the Sun, researchers identified emissions of various cyanide (CN) compounds and neutral nickel (Ni).
Interestingly, iron (Fe) was not detected, implying that nickel is efficiently released by comatose dust particles under solar radiation influence.
The rate of production for these emissions increases significantly as the comet nears the Sun, establishing a strong power-law relationship with its geocentric distance.
These observations indicate that the release of these atoms may stem from low-energy mechanisms, like photon-stimulated desorption or the breakdown of complex organics, rather than the direct sublimation of ice. This distinguishes this interstellar comet from many others within the solar system.
This spectral data not only acts as a snapshot of a transient visitor, but interstellar comets like 3I/ATLAS offer pristine samples from materials formed around other stars. Their limited processing from solar proximity preserves valuable clues about distant protoplanetary disks—the swirling clouds of gas and dust which eventually form planets.
Past interstellar discoveries, such as ‘Oumuamua in 2017 and 2I/Borisov in 2019, have exhibited surprising contrasts. ‘Oumuamua appeared inert, while 2I/Borisov showcased an abundance of carbon monoxide and complex ice.
The new insights from 3I/ATLAS contribute another intriguing layer to this expanding cosmic narrative. Its dusty constitution reveals molecular traits that challenge our understanding of typical comet behavior and introduce novel physics.
3I/ATLAS spectrum from the monitoring campaign spanning July 4 to August 21, 2025. Image credit: Rahatgaonkar et al., doi: 10.3847/2041-8213/ae1cbc.
“If 3I/ATLAS maintains the absence of iron while exhibiting nickel emissions during perihelion, it will set a precedent for observing interstellar comet metal emissions decoupled from traditional refractory trends,” the researchers stated.
“This observation suggests a distinct low-temperature organometallic pathway for nickel in exocomets and may provide fresh perspectives on how disk chemistry, metallicity, and irradiation history affect planetesimal microphysics.”
The parent star of 3I/ATLAS is presumed to be less metallic than other interstellar progenitor stars, yet more metallic than the Sun, indicating no inherent conflict between its estimated age and the presence of iron-peak elements like nickel.
“Regardless of which interpretation is accurate, 3I/ATLAS promises a critical experiment linking metal emissions with volatile activation and particle physics in interstellar bodies.”
“The findings discussed will elevate nickel from being a mere curiosity into a crucial marker for determining both parent chemistry and galactic origins, and set new standards for rapid-response spectroscopy of interstellar objects at the Rubin Observatory and ESO’s Very Large Telescope.”
For further details, see the published findings on December 10, 2025, in the Astrophysics Journal Letter.
_____
Rohan Rahat Gaonkar et al. 2025. Observations of interstellar comet 3I/ATLAS using a very large telescope: From quiescence to luminescence—Dramatic increases in Ni i emissions and initial CN outgassing at extensive heliocentric distances. APJL 995, L34; doi: 10.3847/2041-8213/ae1cbc
Using Enhanced Resolution Imagers and Spectrographs (ERIS) from ESO’s Very Large Telescope (VLT), two teams of astronomers have discovered a protoplanet candidate nestled within a spiral disk surrounding the young star HD 135344B.
This image depicts a spiral disk surrounding Young Star HD 135344b. The observations made using the Enhanced Resolution Imager and Spectrograph (ERIS) identified a candidate planet contributing to the spiral structure in the disk, marked by a white circle. Image credits: ESO/Maio et al.
“While we may never witness the formation of Earth, this is a significant finding,” says Francesco Maio, a doctoral researcher at the University of Florence in Italy and lead author of a paper published in the journal Astronomy and Astrophysics.
Maio and his colleagues identified protoplanet candidates in the surrounding protoplanetary disks of HD 135344b. This F8V star, approximately 11.9 million years old, is situated 135 parsecs (440 light-years) from the Sun, in the Lupus constellation.
The protoplanet is estimated to be twice the size of Jupiter, located at a distance from its host star comparable to that of Neptune from the Sun.
It has been observed maturing at the periphery of the protoplanetary disk as it evolves into a fully-fledged planet.
Similar protoplanets have been detected around other young stars, often exhibiting intricate features such as rings, gaps, and spirals.
Astronomers long suspected that these structures were sculpted by forming planets, clearing away material as they orbit their parent stars.
Until now, however, no one has identified a planet actively shaping these features.
In the discs of HD 135344B, previous observations of swirling spiral arms were made by another team using VLT’s Sphere instrument.
Yet prior observations did not find evidence of any planets forming within this disk.
Utilizing VLT’s ERIS instrument, Maio and his collaborators may have discovered their primary suspect.
They identified a planetary candidate located at the base of one of the spiral arms of the disk, aligning with theoretical predictions about potential planets responsible for such patterns.
“What marks this detection as potentially groundbreaking is our ability to directly observe the signal from the protoplanet, unlike many earlier observations,” he notes.
“This gives us greater confidence in the existence of this planet, as we can see the light it emits.”
This image illustrates possible sub-brown dwarf companions orbiting Young Star V960 Mon. Candidate objects were detected using ESO’s Very Large Telescope (VLT) and the new Enhanced Resolution Imager and Spectrograph (ERIS). The ERIS data is shown in orange, overlaid with prior dusty disk images from VLT’s Sphere instruments (yellow) and ALMA (blue). Image credits: ESO/A. Dasgupta/ALMA/ESO/NAOJ/NRAO/Weber et al.
In a separate study, Anuroop Dasgupta, a doctoral researcher at ESO and Diego Portales University, along with colleagues, observed another young star using the ERIS instrument. V960 is located 1637.7 parsecs (5,342 light-years) away in the Monoceros constellation.
Prior observations using Sphere equipment and large millimeter/sub-millimeter arrays (ALMA) revealed that the material orbiting V960 Mon is shaped into complex spiral arms.
These observations also indicated that large clumps of material around the star undergo gravitational instability, contracting and collapsing—each capable of forming a planet or larger body, thus fragmenting the material.
Dasgupta and his collaborators managed to identify a brown dwarf or sub-brown dwarf companion around V960 Mon.
“Using ERIS, we aimed to discover compact, bright fragments indicative of companions in the disk,” he explains. Their findings are detailed in a paper published in the Astrophysical Journal Letters.
“One potential companion object was found very close to one of the observed spiral arms in the Universe and in ALMA data.”
“This object could represent a planet or a brown dwarf—larger than a planet but lacking sufficient mass to shine like a star.”
“If confirmed, this companion could be the first clear identification of a planet or brown dwarf formed via gravitational instability.”
____
F. Maio et al. 2025. Development of Protoplanet candidates embedded using VLT/ERIS on HD135344B disks. A&A 699, L10; doi:10.1051/0004-6361/202554472
Anuroop Dasgupta et al. 2025. VLT/ERIS observations for the V960 series: dust-embedded sub-brown dwarf objects formed by gravitational instability? ApJL 988, L30; doi: 10.3847/2041-8213/ade996
The astronomer utilizing ESO’s Extremely Large Telescope (VLT) has unveiled a new image of 3i/Atlas, marking it as the third interstellar object documented.
This VLT/FORS2 image, captured on July 3, 2025, depicts interstellar comet 3i/Atlas. Image credit: ESO/O. Hainaut.
3i/Atlas was identified a week ago by the NASA-supported Atlas Survey Telescope in Riojartad, Chile.
Commonly referred to as C/2025 N1 (ATLAS) and A11PL3Z, this comet is approaching from the direction of Sagittarius.
“In contrast to objects within the solar system, its highly eccentric hyperbolic orbit indicates its interstellar origin,” ESO astronomers stated.
Currently, 3i/Atlas is approximately 4.5 AU (670 million km, or 416 million miles) away from the Sun.
Interstellar objects pose no danger to Earth, maintaining a distance of at least 1.6 AU (240 million km, or 150 million miles).
Around October 30, 2025, it will make its closest approach to the Sun at a distance of 1.4 AU (210 million km, or 130 million miles).
“In the VLT time-lapse, you can observe 3i/Atlas moving to the right over approximately 13 minutes,” the astronomer remarked.
“These observations were gathered using FORS2 equipment at the VLT on the night of July 3, 2025, just two days post-discovery of the comet.”
“At the conclusion of the video, all frames are compiled into a single image.
“However, this record will not endure as the comet approaches Earth and becomes less visible.”
“As it currently traverses more than 600 million km from the Sun, 3i/Atlas is heading towards the inner solar system, expected to reach its closest approach to Earth in October 2025,” they noted.
“During that time, 3i/Atlas will be obscured by the Sun, but observations should resume in December 2025.
“Telescopes globally, including the VLT, will persist in monitoring this extraordinary celestial visitor to gather more insights into its structure, composition, and origin.”
Astronomers utilizing ESO’s Extremely Large Telescope (VLT) have captured images of SNR 0509-67.5.
This image, obtained with the multi-unit spectroscopic explorer (Muse) located on ESO’s Extremely Large Telescope (VLT), displays the supernova remnant SNR 0509-67.5. The Calcium shown in blue is arranged in two concentric shells, indicating a double explosion of the star. Image credits: ESO/DAS et al. / Noll et al.
“White dwarfs—small, inert cores resulting from the demise of sun-like stars—are capable of producing what astronomers classify as type Ia supernovae,” states a PhD student from the University of New South Wales University of Canberra.
“Our understanding of the universe’s expansion hinges on these supernovae, which also serve as the primary source of iron on Earth, including in blood.”
“Yet, despite their significance, the mechanisms driving their explosions are still not fully understood.”
All theories surrounding Type Ia supernovae begin with pairs of white dwarf stars.
When one of the stars’ orbits is sufficiently close to its counterpart, it can siphon material from its companion.
According to the most prevalent theory regarding Type Ia supernovae, the white dwarf accumulates matter until it hits a critical mass and then experiences a singular explosion.
However, new research indicates that at least some Type Ia supernovae could be better explained by a series of double explosions occurring before the stars reach this critical mass.
The recent VLT images of SNR 0509-67.5 confirm these predictions.
In this alternative model, the white dwarf forms a helium layer through theft, which becomes unstable and can ignite.
This initial explosion generates a shockwave that moves inward, resulting in another explosion at the core of the star, ultimately leading to the supernova.
Until now, there had been no clear visual proof supporting the occurrence of a double explosion in white dwarfs.
Recent studies have suggested that this process creates identifiable patterns or “fingerprints” on the still-glowing debris from the supernova, surfacing long after the primary explosion.
Research proposes that the remains of such supernovae contain two distinct calcium signatures.
Das and his colleagues have found these fingerprints on the supernova remnants.
“The findings clearly indicate that white dwarfs can explode well before reaching the famous Chandrasekhar limit, demonstrating that the ‘double explosion’ mechanism naturally occurs,” remarks Dr. Ibo Seitenzar, an astronomer at the Heidelberg Institute.
Astronomers were able to identify these calcium layers in SNR 0509-67.5 by employing VLT’s multi-unit spectroscopic explorer (Muse).
This provides compelling evidence that Type Ia supernovae can occur prior to their progenitor white dwarfs reaching critical mass.
“This tangible evidence of double explosions not only aids in resolving historical mysteries but also offers a visual interpretation,” explains Das.
“It’s incredibly satisfying to reveal the intricate workings behind such colossal cosmic explosions.”
The team’s results are published today in the journal Nature Astronomy.
____
P. Das et al. Calcium in the remnants of the supernova as fingerprints of the sub-Chandrasekhar explosion. Nature Astronomy Published online on July 2, 2025. doi:10.1038/s41550-025-02589-5
This VLT/Muse image displays a detailed multi-colored view of NGC 253. Image credit: ESO/Congiu et al.
NGC 253 lies approximately 11.5 million light-years away in the Sculptor constellation.
Commonly referred to as the Silver Coin, Silver Dollar Galaxy, or Sculptor Galaxy, this galaxy was discovered on September 23, 1783, by Caroline Herschel, the sister of William Herschel.
It is one of the brightest members of the Sculptor group of galaxies.
Characterized as a starburst galaxy, it experiences unusually rapid star formation and stellar explosions.
“NGC 253 is one of the largest star-forming galaxies near the Milky Way,” noted ESO astronomer Enrico Kong and his team.
“It also ranks among the largest galaxies in the sky, with apparent dimensions of 42 x 12 arcminutes2.
“With its distinct stellar bars, well-defined spiral arms, and widespread star formation, NGC 253 exemplifies a classic spiral galaxy near the main sequence.”
To create a new image of the galaxy, astronomers dedicated over 50 hours observing it with the VLT’s Muse Instrument.
They needed to stitch together more than 100 exposures to encapsulate an area of approximately 65,000 light-years.
“You can focus on individual regions where stars form at a scale of individual stars, or you can zoom out to view the entire galaxy,” explained Dr. Kathryn Kreckel, an astronomer at the University of Heidelberg.
In their initial data analysis, researchers identified 500 planetary nebulae and regions of gas and dust within NGC 253.
“In areas outside our galaxy, we typically find fewer than 100 detections per galaxy,” remarked Fabian Schuerman, a doctoral student at Heidelberg University.
“Due to the properties of planetary nebulae, they serve as distance markers for host galaxies.”
“By locating the planetary nebulae, we can confirm the distance to the galaxy, which is crucial for other galaxy research.”
“Future projects utilizing maps will investigate gas flows and how their composition influences star formation across this galaxy.”
“It remains a mystery why such a minor process can significantly influence galaxies that are thousands of times larger,” stated Dr. Kong.
New observations of 86 planet-forming disks provide astronomers with a wealth of data and unique insight into how planets form in different regions of the Milky Way.
A planet-forming disk around a young star and its location in the gas-rich clouds of the constellation Taurus, about 600 light-years from Earth. Scientists observed a total of 43 stars in the Taurus region, all of which are pictured here (although planet-forming disks were detected in only 39 of these targets) ).Image credit: ESO / Galfi other. /Iras.
More than 5,000 exoplanets have been discovered to date, many of them in planetary systems significantly different from our solar system.
To understand where and how this diversity occurs, astronomers need to look at the dust- and gas-rich disks that envelop young stars: the cradles of planet formation. These are most commonly found in the giant gas clouds in which the stars themselves are forming.
As with mature planetary systems, new images from ESO's Very Large Telescope (VLT) show the amazing diversity of planet-forming disks.
“Some of these disks show huge spiral arms, probably driven by a complex ballet of orbiting planets,” said Christian Ginski, an astronomer at the University of Galway.
“Some show rings or large cavities formed by planet formation, while others appear smooth and almost dormant amidst this hustle and bustle of activity,” said Antonio Galfi, an astronomer at the Arcetri Astrophysical Observatory. he added.
The authors studied a total of 86 stars across three different star-forming regions in the Milky Way. Taurus and Chameleon I are both about 600 light-years from Earth, and Orion is a gas-rich cloud about 1,600 light-years from us. It is known as the birthplace of several stars more massive than the Sun.
In the Orion cloud, we found that stars in groups of two or more are less likely to have large disks that form planets.
This is an important result given that, unlike our Sun, most stars in our galaxy have companion stars.
In addition to this, the uneven appearance of the disk in this region suggests that there may be a giant planet embedded within it, which could cause the disk to become distorted or misaligned. there is.
Planet-forming disks can extend to distances hundreds of times the distance between Earth and the Sun, but because of their location hundreds of light-years from us, they appear like tiny needles in the night sky. I can see it.
To observe the protoplanetary disk, astronomers used the VLT's Spectropolarimetric High-Contrast Exoplanet Research Equipment (SPHERE).
Additional data was obtained using VLT's X-SHOOTER instrument, allowing researchers to determine how young the star is and how massive it is.
The Atacama Large Millimeter/Submillimeter Array (ALMA) has helped us understand more about the amount of dust around some stars.
Per Gunnar Vallegord, a PhD student at the University of Amsterdam, said: “The process that marks the beginning of the journey towards the formation of planets and, ultimately, the formation of life in our solar system could not be more beautiful. It's almost poetic that it is.”
A dynamically active planetary system orbits a significant portion of the white dwarf. These stars often exhibit surface metals accreted from a disk of debris. However, the complete journey of a planetesimal from its star-grazing orbit to its final dissolution in its host star is poorly understood. In a new paper, Astrophysics Journal Letter astronomers report the discovery that stars exist that are contaminated with cold metals. WD 0816-310 It cannibalized heavy elements from a planetary body as large as the dwarf planet Vesta.
WD 0816-310 is a magnetic white dwarf star located 63 light-years away in the constellation Papis. Image credit: L. Calçada / ESO.
Dr Stefano Vanullo, an astronomer at the Armagh Observatory and Planetarium, said: 'It is common for some white dwarfs – slowly cooling embers of stars like our Sun – to cannibalize parts of planetary systems. known,” he said.
“Now we find that the star's magnetic field plays a key role in this process, causing scars on the white dwarf's surface.”
The metal signatures the researchers observed on WD 0816-310 are concentrations of metal imprinted on the white dwarf's surface.
Professor Jay Farihi of University College London said: “These metals come from fragments of a planet the size of, or possibly even larger than, Vesta, which at about 500 kilometers in diameter is the second largest asteroid in the solar system. I have proven that.”
They also relied on archival data from VLT. X shooter instrument This is to confirm the survey results.
The authors noticed that the strength of the metal detections changed as the star rotated, indicating that the metals were concentrated in specific areas on the white dwarf's surface, rather than being spread smoothly across the surface. Suggests.
They also found that these changes were synchronized with changes in the white dwarf's magnetic field, indicating that this metallic scar is located at one of its magnetic poles.
Taken together, these clues indicate that the magnetic field funneled metal into the star, creating the scar.
“Surprisingly, the material was not evenly mixed on the star's surface, as theory predicted. Instead, this scar was a concentrated patch of planetary material that guided falling debris. “We've never seen anything like this before,” said John Landstreet, a professor at Western University.
“ESO offers a unique combination of capabilities needed to observe faint objects like white dwarfs and make sensitive measurements of the star's magnetic field,” Vanullo said.
_____
Stefano Vanullo other. 2024. Discovery of magnetically induced metal accretion on contaminated white dwarfs. APJL 963, L22; doi: 10.3847/2041-8213/ad2619
This website uses cookies so that we can provide you with the best user experience possible. Cookie information is stored in your browser and performs functions such as recognising you when you return to our website and helping our team to understand which sections of the website you find most interesting and useful.
Strictly Necessary Cookies
Strictly Necessary Cookie should be enabled at all times so that we can save your preferences for cookie settings.
