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Two Protoplanets Forming in Dusty Disk Around Nearby Young Star: Key Discoveries in Planet Formation

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Astronomers utilizing ESO’s Very Large Telescope (VLT) and VLT Interferometer (VLTI) in Chile have made groundbreaking discoveries by directly observing two giant gas planets forming within a planet-forming disk around the star Whispit 2. This research offers one of the most detailed insights into planetary system formation to date, highlighted by distinctive gaps and rings of surrounding material, which suggest the likelihood of additional alien worlds in the vicinity.

Images captured by ESO’s Very Large Telescope illustrate a young planetary system orbiting the star WISPIT 2. Image credit: ESO / Lawlor and colleagues.

“WISPIT 2 represents our clearest glimpse into the early stages of planetary formation,” stated Dr. Chloe Lawler, a researcher from Galway University.

“This discovery enables us to study entire planetary systems, rather than just individual planets in isolation,” noted Dr. Christian Ginski, also associated with the University of Galway.

“Such observations are crucial for enhancing our understanding of how nascent planetary systems evolve into mature systems like our own,” he added.

The first protoplanet found in the WISPIT 2 system, designated WISPIT 2b, was identified last year and has a mass nearly five times that of Jupiter, orbiting at a distance approximately 60 times that between the Earth and the Sun.

“Discovering this new world in formation showcases the remarkable capabilities of our current astronomical instruments,” commented Dr. Richelle van Capelveen from the Leiden Observatory.

Subsequent observations detected additional objects near WISPIT 2, with measurements from the VLT and VLTI confirming their planetary nature.

The newly identified planet, WISPIT 2c, is located four times closer to its host star and is twice as massive as WISPIT 2b.

Both planets are gas giants, akin to the outer planets in our solar system.

To validate WISPIT 2c, astronomers employed the SPHERE instrument on the VLT, followed by VLTI’s GRAVITY+ instrument to confirm it as a planet.

“Our study leveraged recent enhancements to GRAVITY+, which were essential for detecting such a clear planet in proximity to its star,” stated Dr. Guillaume Bourdaro from the Max Planck Institute for Extraterrestrial Physics.

Both planets orbiting WISPIT 2 manifest in distinct gaps within the surrounding dust and gas disk, a phenomenon caused by each planet’s gravitational influence.

The material remaining around each gap forms unique dust rings within the disk composition.

In addition to the gaps hosting the two planets, at least one smaller gap exists further out in the WISPIT 2 disk.

“This narrower and shallower gap may indicate the presence of a third planet, possibly with a mass akin to Saturn,” Lawler speculated.

The findings are set to be detailed in an upcoming article in the Astrophysical Journal Letters.

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Chloe Lawler and colleagues. 2026. Direct spectroscopy confirmation of the young embedded protoplanet WISPIT 2c. APJL 1000, L38; doi: 10.3847/2041-8213/ae4b3b

Source: www.sci.news

JWST Unveils Insights into Dusty Star-Forming Galaxies – Sciworthy

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The origin of the universe is cloaked in cosmic dust. This vast expanse is teeming with tiny particles, ranging from a handful of molecules to micrometers – a scale of up to a millionth of a meter, or a hundred thousandth of an inch. From the dawn of the universe to the present day, massive clouds of gas and dust have accumulated and collapsed, giving birth to stars and galaxies. By investigating these particles, scientists can unlock secrets about the early universe. However, dust often obscures many interstellar objects from telescopes, limiting our understanding of deep space.

Astronomers are especially intrigued by a class of distant cosmic entities known as dust-enshrouded star-forming galaxies (DSFGs), which are prolific in star production. These ancient galaxies create over 100 stars annually—nearly ten times the rate of the Milky Way—but their visible light is entirely masked by dust. To decipher high-resolution data, astronomers employ a method known as astronomy to unearth the characteristics of these DSFGs. It’s akin to examining a high-definition 4K image, yet from the far reaches of outer space. Until recently, no equipment could successfully resolve DSFGs. This changed with the advent of the James Webb Space Telescope (JWST).

An international team of astronomers has recently succeeded in resolving 22 DSFGs using the JWST’s near-infrared camera, NIRCam. This advanced instrument can observe galaxies at wavelengths between 0.6 to 5 micrometers (approximately 1/5 millionth of a meter, or 2/1000ths of an inch). Astronomers leverage these high-resolution observations to navigate the dust enveloping DSFGs.

The research team utilized seven distinct filters in NIRCam to isolate specific wavelengths or colors of light from each galaxy. Each filter reveals different physical properties, including the galaxies’ size, shape, lumpiness, mass, and star formation rates. No single filter can capture all properties simultaneously; astronomers must also adjust their filters in accordance with the distance between the galaxy and Earth. Due to the universe’s expansion, older, more distant galaxies like the DSFG are receding from our own, causing the light waves we capture to stretch—a phenomenon known as redshift.

With the high-resolution data, the team classified DSFGs into three categories based on their visual traits. Type I galaxies create stars across their entirety, Type II galaxies concentrate star formation in their cores, while Type III galaxies generate stars only in their outer regions, known as the galactic disk. Astronomers studying cosmic history focus on areas where stars are not forming due to rapid cooling, identifying Type II and Type III galaxies. The study found 10 Type I galaxies, five Type II galaxies, and seven Type III galaxies among the DSFGs analyzed.

The team further explored the internal characteristics of each galaxy to unravel general trends within each type. To gauge their mass and star formation rates, astronomers employed models based on patterns of light emitted by the DSFGs, discovering that their sizes range from 30 billion to 300 billion times that of the Sun. Notably, the most massive DSFGs are smaller than the Milky Way and generate between 25 and 500 stars annually, located between 10 billion and 18 billion light-years from Earth.

The researchers also analyzed the shapes of these galaxies, noting that the more distant and older a galaxy is, the more fragmented its form appears. This fragmentation suggests that the high-redshift DSFGs are in a phase of forming tightly packed collections of stars, a structure known as a bulge. These galaxies may eventually experience quenching at their centers, morphing into Type III galaxies. Furthermore, scientists uncovered a previously unnoticed feature across many galaxies: they exhibit polarization, indicating potential past mergers with other galaxies.

The research team concluded that the high-resolution data provided by JWST can unveil hidden features within DSFGs, aiding astronomers in piecing together their past and predicting future developments. They advocate for upcoming researchers to utilize JWST data to test hypotheses regarding the evolution and characteristics of these fascinating galaxies.


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Source: sciworthy.com

Saturn’s Rings Create a Massive Dusty Donut Encircling the Planet

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A stunning view of Saturn and its rings as seen by the Cassini spacecraft

NASA/JPL-Caltech/Space Science Institute

New findings indicate that dust particles from Saturn’s rings are extended farther above and below the planet than previously assumed, implying that the rings might be shaped like large, dusty donuts.

The central structure of Saturn’s rings is remarkably thin, stretching out for tens of thousands of kilometers while only measuring around 10 meters in height, which gives Saturn its iconic look from Earth. However, variations exist, such as the outer E-ring that is inflated and replenished by ice ejected from Saturn’s moon Enceladus, which has an ocean beneath its surface.

In a recent study, Frank Postberg and his team at the Free University of Berlin examined data from NASA’s Cassini spacecraft, which completed 20 orbits in its final year of operation in 2017. During these orbits, the spacecraft took a steep trajectory through the rings, starting from a distance up to three times Saturn’s radius and moving downwards towards three times Saturn’s radius.

At the height of Cassini’s orbital path, its spectrometer, known as the Cosmic Dust Analyzer, detected hundreds of tiny rock particles with a chemical makeup similar to those found in the iron-deficient main rings. “This spectral type is genuinely unique within the Saturn system,” Postberg stated.

“While more material is near the surface of the rings, it is still astonishing that these particles are found so far above and below the ring surface,” he added.

Postberg and his collaborators determined that to reach heights greater than 100,000 kilometers from the main ring, the particles must be traveling at speeds exceeding 25 kilometers per second to break free from Saturn’s gravitational and magnetic forces.

Postberg noted that the exact mechanism achieving such speeds remains uncertain. The simplest explanation might be that a minor meteorite strikes the ring, scattering particles; however, this does not generate debris quickly enough.

New research suggests that when micrometeorites impact Saturn’s rings, they could generate sufficiently high temperatures to vaporize the rocks, implying that Saturn’s rings are older than once believed. Postberg and his team propose that this vaporized rock could exit the ring at much higher speeds than expected and then condense far from the planet.

It is surprising to find dust at such distances from the main ring. According to Frank Spahn from the University of Potsdam in Germany, who was not part of the study, this is significant because the particles in Saturn’s primary rings are small, collide rarely, and are sticky, leading to collisions that behave more like snowballs colliding than like billiard balls.

Micrometeorite impacts are prevalent throughout the solar system; hence, similar processes might be occurring on other ringed planets like Uranus. “If a ring of ice experiences a high-velocity impact, this phenomenon could be widespread; we would expect analogous dust rings above and below the other rings,” Postberg concluded.

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Source: www.newscientist.com

Hubble Captures Stunning Image of Dusty Spiral Galaxy NGC 7496

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NGC 7496 is a barred spiral galaxy situated roughly 24 million light-years away in the Taurus constellation.

This Hubble image captures barred spiral galaxy NGC 7496 in the constellation Hyuri, located approximately 24 million light-years away. Image credits: NASA / ESA / Hubble / R. Chandar / J. Lee / PHANGS-HST team.

NGC 7496 was discovered by British astronomer John Herschel on September 5, 1834.

The galaxy is also identified as ESO 291-1, LEDA 70588, and IRAS 23069-4341, and spans approximately 70,000 light-years in diameter.

NGC 7496 belongs to the NGC 7582 group, which comprises about 10 large galaxies.

This galaxy is classified as a Type II Seyfert galaxy, notable for a high star formation rate.

At its center lies an active galactic nucleus containing a supermassive black hole primarily consuming gas.

According to Hubble astronomers, “Hubble observed NGC 7496 for the first time as part of the Physics at High Angular Resolution of the Nearby GalaxieS (PHANGS) program.”

“Alongside the NASA/ESA Hubble Space Telescope, this initiative utilizes the capabilities of various powerful observatories, including the Atacama Large Millimeter/Submillimeter Array, ESO’s Very Large Telescope, and the NASA/ESA/CSA James Webb Space Telescope.”

“NGC 7496 was the inaugural galaxy in the PHANGS sample to be observed by Webb.”

“Each of these observatories offers a unique perspective on this extensively studied galaxy.”

“With its exceptional ultraviolet capabilities and high resolution, Hubble’s observations reveal young star clusters emitting high-energy radiation.”

“Hubble’s insights into NGC 7496 will assist in determining the ages and masses of these young stars, as well as the degree to which their light is obscured by dust.”

“Previous Hubble images of NGC 7496 were released in 2022,” they noted.

“Today’s image incorporates fresh data showcasing the galaxy’s star clusters amid glowing red clouds of hydrogen gas.”

Source: www.sci.news

Hubble Discovers Dusty Clouds in the Tarantula Nebula

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The stunning new image from the NASA/ESA Hubble Space Telescope reveals intriguing details of the Tarantula Nebula, a dynamic region of star formation located in the Large Magellanic Cloud.

This Hubble image showcases part of the Tarantula Nebula, located about 163,000 light years away in the Dorado constellation. The colorful image is a composite of various exposures captured by Hubble’s Wide Field Camera 3 (WFC3) across ultraviolet, near-infrared, and spectral optical ranges. It is based on data collected using four different filters. Colors have been assigned by applying various hues to each monochromatic image produced by the individual filters. Image credits: NASA/ESA/Hubble/C. Murray.

The Tarantula Nebula is situated roughly 163,000 light years from the southern constellation of Dorado.

Also known as NGC 2070 or 30 Dorados, this nebula is part of the expansive Magellanic Cloud, which is one of our closest galactic neighbors.

The nebula’s brilliant glow was first observed in 1751 by French astronomer Nicolas Louis de Lacaille.

At its core lies some of the most massive stars known, with some reaching up to 200 solar masses, making this region ideal for studying how gas clouds collapse under gravitational forces to give rise to new stars.

“The Tarantula Nebula is the largest and brightest area of star formation not only within the Large Magellanic Cloud but also among the entire group of nearby galaxies that include the Milky Way,” astronomers associated with Hubble stated.

“Within the nebula are some of the most massive stars discovered, some of which are approximately 200 times the mass of our Sun.”

“The scene depicted here is located far from the nebula’s center, where the superstar cluster known as R136 resides, but is quite close to a rare star called the Wolf-Rayet Star.”

“The Wolf-Rayet star is an enormous star that has shed its outer hydrogen layers; it is extremely hot, bright, and generates a dense, powerful wind,” they elaborated.

The Tarantula Nebula is frequently observed by Hubble, and its multi-wavelength capabilities play a crucial role in capturing the intricate details of the nebula’s dusty cloud formations.

“The data used to produce this image come from an observational program known as Scylla, which is named after the multi-faceted sea monster from the Greek mythology of Ulysses,” the astronomer noted.

“The Scylla program was developed to complement another Hubble observational initiative called Ulysses (the Ultraviolet Legacy Library of Young Stars as a fundamental criterion).”

“While Ulysses focuses on giant young stars in the small Magellanic Cloud, Scylla explores the gas and dust structures surrounding these stars.”

Source: www.sci.news