unexpected mineral found in Ryugu asteroid

Rare Mineral Found in Ryugu Asteroid Challenges Solar System Formation Theories

Hayabusa2 Mission Uncovers Crucial Clues from Ryugu

Pristine Samples and Their Importance

The untouched samples retrieved from asteroid Ryugu by the Hayabusa2 mission on 6 December 2020 have been crucial in refining our knowledge of primitive asteroids and solar system formation. Ryugu, a C-type asteroid, comprises rock akin to CI chondrite meteorites—rich in carbon and bearing clear signs of past aqueous alteration.

Discovery of an Unexpected Mineral in Ryugu

Identification of Djerfisherite

A team of researchers from Hiroshima University has identified the mineral djerfisherite—a potassium-bearing iron-nickel sulphide—within a grain from asteroid Ryugu. Its discovery is entirely unexpected, as such a mineral is not thought to form under the environmental conditions Ryugu is believed to have experienced.

The Journal Meteoritics & Planetary Science has published the team's findings.

Expert Insight from Dr. Masaaki Miyahara

"Ordinarily, djerfisherite is encountered in significantly reduced settings, such as those characteristic of enstatite chondrites. Its absence in CI chondrites and Ryugu material has been consistent—until now," explained Dr. Masaaki Miyahara, first and corresponding author and associate professor at Hiroshima University.

Challenging Current Understanding of Primitive Asteroids

Exotic Conditions or Early Solar System Transport?

"Its presence is akin to discovering a tropical seed embedded within Arctic ice—suggesting either a surprisingly exotic local condition or significant transport across vast distances in the early solar system."

Weathering Experiments and Analysis

Miyahara's research group had been conducting experiments to investigate how Ryugu grains respond to terrestrial weathering. During FE-TEM analysis, they identified djerfisherite in grain number 15 from sample plate C0105-042.

Implications for Solar System Formation Models

"The presence of djerfisherite within a Ryugu grain implies that substances with disparate origins might have mingled in the early solar system, or that Ryugu encountered previously undetected, chemically diverse environments. This discovery contests the assumption of Ryugu's compositional uniformity and raises intriguing questions regarding the complexity of primordial asteroids," explained Miyahara.

Thermal and Chemical History of Ryugu's Parent Body

Formation in the Outer Solar System

Ryugu originated from a larger celestial precursor, which came into being around 1.8 to 2.9 million years post-solar system formation. Scientists surmise this body took shape in the solar system's colder outer zones, rich in frozen water and carbon dioxide.

Radioactive Heating and Ice Melting

Within the parent body, the decay of radioactive isotopes produced heat that led to the melting of ice roughly 3 million years post-formation. During this period, temperatures are believed to have remained below 50°C.

Comparison with Enstatite Chondrites

Conversely, the parent bodies of enstatite chondrites, which exhibit the presence of djerfisherite, are believed to have originated closer to the Sun. Thermodynamic assessments indicate the mineral emerged from condensation within high-temperatures gases.

Experimental Confirmation

In addition, controlled hydrothermal experiments suggest that djerfisherite may from through chemical interactions between postassium-laden fluids and Fe-Ni sulphides at elevated temperatures exceeding 350 °C.

Hypotheses and Future Directions

Two Possible Origins for Djerfisherite in Ryugu

Two explanations were offered for the mineral's inclusion within the Ryugu grain: either it originated elsewhere and was introduced during the parent body's creation, or it formed locally as a result of thermal conditions exceeding 350°C.

Isotopic Analysis to Follow

Initial findings suggest that the hypothesis favouring intrinsic formation is the more probable explanation. Subsequent work will involve isotopic analysis of this and additional Ryugu grains to elucidate their provenance.

Toward a Deeper Understanding of Planetary Formation

Broader Scientific Goals

"Our ultimate objective is to piece together the early mixing events and thermal developments that influenced minor celestial bodies such as Ryugu, thereby enhancing our insight into planetary genesis and mterial movement within the nascent solar system," Miyahara remarks.

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astronomers discover new ultracompact am cvn

Astronomers Discover New Ultracopact AM CVn Binary with Rare Outbursts-TCP J07222683+6220548 Revealed

Introduction to the New Ultracompact binary System

Astronomers from across the world have detected a fresh ultracompact binary system of the AM CVn variety, which displays occasional outbursts. Full details of TCP J07222683+6220548 were released on 27 May in a paper on the arXiv preprint server.

Understanding Cataclysmic Variables (CVs)

Cataclysmic Variables (CVs) are binary systems comprising a white dwarf and an ordinary stellar companion, from which the former draws in material. Their luminosity has been observed to surge erratically before settling back into a dormant phase.

The AM CVn Class

The AM CVn Class—taking its name from AM Canum Venaticorum—comprises a rare breed of cataclysmic variable. Here, a white dwarf in helium-dominated, hydrogen-scarce material from a closely orbiting companion. Their orbits are notably brief, lasting between five minutes and around sixty minutes.

Discovery of the New AM CVn System

A team of astronomers headed by Alexander Tarasenkov of the Russion Academy of Sciences has announced the discovery of anew AM CVn system, observed on 20 January 2025 during the New Milky Way (NMW) survey. The object exhibited a seven-day outburst, followed by several episodes of rebrightening from January through March. Subsequent observation confirmed its classification as an AM CVn.

Characteristics of TCP J07222683+6220548 (J0722)

Location and Spectral Profile

The study notes that TCP J07222683+6220548, referred to as J0722, lies at an approximate distance of 1,874 light years. Its spectral profile features a blue continuum with distinct broad helium absorption lines, absent of Balmer hydrogen lines—hallmarks of an AM CVn system undergoing outburst.

Outburst Brightness and Accretion Disc Orientation

J0722's outburst reached a peak brightness of 12.45 magnitude, ranking it among the most luminous AM CVn events recorded to date. The absolute magnitude, measured at 3.4 implies the accretion disc is likely being observed nearly face-on, enhancing its perceived luminosity.

Observations of Photometric Variations

Periodic Modulation and Positive Superhumps

Researchers observed a recurring modulation in J0722's light curve, with a period of roughly 46.87 minutes. This variation is believed to signify positive superhumps, a photometric feature common to certain dwarf novae and similar systems.

Superhums During Re-brightening

The scientists observed that superhumps became distinctly apparent during J0722's first re-brightening phase, occurring between days 18 and 24 post-outburst. They reported no significant variation in the superhump period.

Summary and Future Directions

summarizing their results, the team noted the strong similarity between J0722's outburst pattern and those of long-period AM CVn binaries, reinforcing the call for further observational campaigns.

Importance of Follow-Up Monitoring

According to the scientists, AM CVn systems without thorough post-outburst monitoring could remain hidden within the latest catalogue of cataclysmic variables.

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nuclear reaction neutron star nanomaterials

First Ever Nuclear Reaction in Neutron Star Remnants Measured Using Nanomaterials

A Breakthrough in Astrophysics and Nuclear physics

Physicists have successfully observed a nuclear reaction that takes place during neutron star collisions, offering experimental data for a process that was once purely theoretical. this research, conducted by the University of Surrey, sheds light on the creation of the universe's heaviest elements and may lead to breakthroughs in nuclear reactor technology.

Historic First Measurement of a Weak r-Process Reaction

The ⁹⁴Sr(α,n)⁹⁷Zr Nuclear Reaction

In collaboration with the University of York, University of Seville, and TRIUMF—Canada's national particle accelerator center—researchers have achieved a historic milestone: the first direct measurement of a week r-process reaction cross-section using a radioactive ion beam. This study focused on the ⁹⁴Sr(α,n)⁹⁷Zr reaction, where strontium-94 absorbs an alpha particle, emits a neutron, and transforms into zirconium-97.

This research has been featured in Physical Review Letters.

Significance of the Weak r-Process in Element Formation

Dr. Matthew Williams, lead author from the University of Surrey, explained, "The weak r-process is fundamental to the formation of heavy elements, as evidenced in ancient stars—celestial fossils preserving the chemical imprints of a singular cataclysmic event, such as a supernova or neutron star merger. This study provides the first direct experimental data to validate models that, until now, were purely theoretical."

Innovative Use of Nanomaterials in Nuclear Experiments

Developing Helium-Based Nano-Targets

Researchers at the University of Seville pioneered a novel nano-material approach to enable the experiment, embedding helium within ultra-thin silicon films. This innovation created billions of microscopic helium bubbles, each measuring only a few tens of nanometers, overcoming the challenge of working with helium—a noble gas that neither reacts nor solidifies.

Utilizing TRIUMF's Advanced Radioactive Ion Beam Technology

Leveraging TRIUMF's cutting-edge radioactive ion beam technology, the team accelerated short-lived strontium-94 isotopes into these specialized targets, enabling them to probe nuclear reactions under astrophysical conditions akin to those in extreme cosmic environments.

Implications for Nuclear Physics and Reactor Design

Dr. Williams remarked, "This groundbreaking achievement bridges astrophysics and nuclear physics, marking the first application of nanomaterials in this context and unlocking promising new avenues for nuclear research."

Advancing Nuclear Reactor Technology

"Beyond its astrophysical significance, understanding the behavior of radioactive nuclei is essential for advancing nuclear reactor design. These nuclei are continuously generated in reactors, yet their reactions have remained challenging to study. Such data are vital for optimizing reactor longevity, predicting component replacement intervals, and developing next-generation, high-efficiency systems."

Future Research and Broader Implications

Future research will integrate these findings into astrophysical models, providing deeper insights into the formation of the universe's heaviest elements. Continued exploration of these processes could enhance our understanding of both the extreme physics governing neutron star collisions and their broader implications for nuclear technology.

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wolf rayet 104 pinwheel star cosmic mystery

Wolf-Rayet 104's Pinwheel Star: A Cosmic Mystery Unraveled

Introduction

New research suggests that the enigmatic Wolf-Rayet 104 "pinwheel star" is more complex than previously believed, yet even less likely to be the catastrophic "death star" once theorized.

WR 104: A Binary System with a Rotating Dust Pinwheel

A study led by W. M. Keck Observatory Instrument Scientist Grant Hill has confirmed a long-held hypothesis: WR 104 consists of a binary system of massive stars orbiting each other every eight months. Their intense stellar winds collide, forming a rotating dust pinwheel that radiates in the infrared and shares the system's orbital period.

Discovery of WR 104's Pinwheel Structure

First identified at Keck Observatory in 1999, WR 104's pinwheel structure captivated astronomers with its striking imagery. The system comprises:

• A Wold-Rayet star an evolved, massive star emitting carbon-enriched winds.
• A more massive but less evolved OB star, whose wind remains predominantly hydrogen.

Formation of the Dust Spiral and its GRB Connection

Astrophysicists suggest that wind collisions in such systems facilitate hydrocarbon formation, commonly termed "dust" in astronomy. WR 104 gained attention not only for this process but also for its potential as a gamma-ray burst (GRB) source.

Early Theories on WR 104's Orientation

Early models of its pinwheel formation suggested an orientation in the plane of the sky, resembling a top-down view of a rotating garden hose.

This alignment suggested that the rotational axes of both stars could be oriented toward Earth.

The "Death Star" Hypothesis

If one of these stars were to undergo a supernova, the resulting explosion might produce a gamma-ray burst (WRB) directed along its polar axis. Given WR 104's location within our own galaxy and its perceived alignment with Earth, it was doubbed the "Death Star."

Video

An artist's depiction of WR 104, initially discovered at Keck Observatory in 1999. This binary system features a Wolf-Rayet star, emitting a strong carbon-rich wind (shown in yellow) and an OB star, whose wind is predominantly hydrogen (shown in blue). The collision of these winds forms a swirling hydrocarbon "dust" spiral. Credit: W. M. Keck Observatory/Adam Makarenko.

New Spectroscopic Analysis Reveals Unexpected Findings

Hill's study, published in the Monthly Notices of the Royal Astronomical Society, leverages spectroscopic data from three Keck Observatory instruments—LRIS, ESI, and NIRSPEC. By analyzing these spectra, he measured the velocities of both stars, determined their orbital parameters, and identified spectral signatures from colliding stellar winds.

However, his findings revealed an unexpected and significant discovery.

The Orbit Misalignment Mystery

"From our vantage point on Earth, the pinwheel dust spiral appears to be face-on, rotating in the plane of the sky, leading to the reasonable assumption that the two stars orbit similarly," Hill explains. "Initially, I expected to focus on the colliding winds, assuming a face-on orbit as a given. However, my findings revealed an unexpected result—the orbit is inclined by at least 30 to 40 degrees."

While this finding alleviates concerns about a nearby GRB directed at Earth, it presents a significant challenge.

Key Questions Raised by the Discovery

• How can the dust spiral and the orbital plane exhibit such a pronounced misalignment?
• Could additional physical mechanisms be influencing the formation of the dust plume?

WR 104 Continues to Surprise

"This discovery exemplifies how astronomical research often unveils surprises we never anticipated," Hill observes.

Each answer leads to new questions, deepening our understanding of physics and the cosmos. WR 104 still holds more surprises for us.

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mysterious galactic core dark matter discovery

Mysterious Galactic Core Energy May Reveal a New Type of Dark Matter

Introduction

The enigmatic event at the center of our galaxy could potentially be caused by an alternative type of dark matter.

Dark matter, an elusive and unobservable substance potentially constituting 85% of the universe's mass, remains one of the most profound scientific pursuits.

New Findings on Dark Matter in the Milky Way

Pioneering research brings scientists a step closer to deciphering the enigma of dark matter, suggesting a novel candidate may drive unexplained chemical reactions in the Milky Way.

A Mystery in the Galactic Core: Positively Charged Hydrogen

Dr. Shyam Balaji, a Postdoctoral Research Fellow at King's College London and a lead author of the study, states: "At the heart of our galaxy lie vast clouds of positively charged hydrogen—an enduring mystery for decades, as hydrogen gas is typically neutral. What mechanism provides the energy necessary to dislodge electrons and create this ionization?"

The energy emission detected in this region of our galaxy indicate a persistent and dynamic energy source.

Could Dark Matter Be Lighter Than Previously Theorized?

Our data suggests that this phenomenon could be driven by a much lighter form of dark matter than currently theorized.

Challenges to the WIMP Model

The leading hypothesis for dark matter suggests it comprises Weakly Interacting Massive Particles (WIMPs), a class of particles that barely interact with ordinary matter, rendering them incredibly elusive.

Today's publication in Physical Review Letters suggests a paradigm shift, bringing renewed focus to a low-mass dark matter candidate that challenges the WIMP-dominated narrative.

A New Explanation: Low-Mass Dark Matter Collisions

According to the study, these lightweight dark matter particles may collide and annihilate, leading to the formation of charged particles capable of ionizing hydrogen gas.

Could Cosmic Rays or WIMPs Explain This Phenomenon?

Earlier explanations for this ionization process centered on cosmic rays—high-energy particles traversing the universe. However, observational data from the Central Molecular Zone (CMZ) suggest that the detected energy signatures are insufficient to be attributed to cosmic rays. Similarly, Weakly Interacting Massive Particles (WIMPs) do not appear capable of driving this phenomenon.

A Slower, Low-Mass Energy Source

The researchers concluded that the energy source driving the annihilation process must be:

• Slower than cosmic rays
• Possess a lower mass than WIMPs

A New Approach to Studying Dark Matter

Dr. Balaji stated, "The quest to uncover dark matter is one of the greatest pursuits in modern science, yet most experiments are conducted on Earth. By analyzing gas within the CMZ through a novel observational approach, we can directly investigate its origins. The data suggests that dark matter may be significantly lighter than previously assumed."

Implications for Galactic Phenomena

Unraveling the mystery of dark matter is a cornerstone of fundamental physics, yet most experiments remain Earth-bound, passively awaiting its detection. By examining the hydrogen gas at the heart of our Milky Way, the CMZ offers promising insights that may bring us closer to uncovering dark matter's true nature.

The 511-keV Emission Line and Dark Matter

This discovery could provide a unified explanation for broader galactic phenomena, including:

• The enigmatic 511-keV emission line observed at the Milky Way's core
• A distinctive X-ray signature that may also originate from low-mass dark matter interactions producing charged particles.

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small magellanic cloud star formation

Small Magellanic Cloud Observations Reveal Clues to Early Universe Star Formation

Introduction: The Birth of Stars in Stellar Nurseries

Stars are born in stellar nurseries, vast regions of gas and dust where the particles condense to create new stars. These molecular clouds can span hundreds of light-years, giving birth to thousands of stars. Although technological advancements and observation tools have provided significant insight into the stellar lifecycle, certain aspects, such as the formation of stars in the early universe, remain uncertain.

New Insights from the Small Magellanic Cloud

In a recent Astrophysical Journal publication, scientists from Kyushu University, working alongside Osaka Metropolitan University, uncovered evidence that stars in the early universe may have originated in diffuse, "Fluffy" molecular clouds. This conclusion, drawn from Small Magellanic Cloud observations, provides a novel perspective on stellar formation over cosmic time.

Understanding Molecular Clouds and Star Formation

Filamentary Structure of Molecular Clouds

In the Milky Way, molecular clouds responsible for star formation exhibit an elongated, filamentary structure approximately 0.3 ligh-years in width. Astronomers posit that our solar system originated similarly, with a vast filamentary molecular cloud fragmenting into a molecular cloud core. Over hundreds of thousands of years, gravitational forces accumulated gas and matter within these cores, ultimately giving rise to a star.

Challenges in Understanding Early Star Formation

"Our knowledge of star formation continues to evolve, yet deciphering how stars emerged in the early universe presents an even greater challenge," says Kazuki Tokuda, a Postdoctoral Fellow at Kyushu University's Faculty of Science and the study's lead author.

The Role of Heavy Elements in Early Universe Star Formation

In the early universe, hydrogen and helium dominated, while heavier elements emerged later in massive stars. Although direct observation of early star formation is impossible, we can study regions with conditions resembling those of the early cosmos.

Observations of the Small Magellanic Cloud (SMC)

Why the SMC is a Key Research Target

The research team focused on the Small Magellanic Cloud (SMC), a dwarf galaxy approximately 20,000 light-years from Earth. With only one-fifth of the heavy elements found in the Milky Way, the SMC closely mirrors the conditions of the early universe from 10 billion years ago. However, limited spatial resolution has made it challenging to determine whether its molecular clouds exhibit filamentary structures.

Using ALMA Telescope to Study the Small Magellanic Cloud

The ALMA radio telescope in Chile provided the necessary resolution to examine the Small Magellanic Cloud (SMC) in greater detail, enabling scientists to assess the existence of filamaentary molecular clouds.

Key Findings from Molecular Cloud Data Analysis

"Our analysis encompassed data from 17 molecular clouds, all of which contained nascent stars with masses approximately 20 times that of our Sun," Tokuda explains. "Around 60% of these clouds exhibited a filamentary structure with an average width of 0.3 light-years, while the remaining 40% displayed a more diffuse, "Fluffy" morphology. Additionally, the filamentary clouds had higher internal temperatures compared to their fluffy counterparts.

Understanding the Transition from Filamentary to Fluffy Clouds

Temperature Differences and Evolution

The temperature disparity between filamentary and fluffy clouds is likely attributable to their formation timeline. Initially, all molecular clouds exhibited a filamentary structure with elevated temperatures due to inter-cloud collisions. At higher temperatures, turbulence within the cloud remains minimal. However, as the cloud cools, the kinetic energy of infalling gas induces greater turbulence, disrupting the filamentary configuration and leading to a more diffuse, "Fluffy" morphology.

Impact on Star Formation and Planetary System Development

A molecular cloud that preserves its filamentary structure is more likely to fragment along its elongated axis, leading to the formation of multiple low-mass stars, such as our skin, accompanied by planetary systems. Conversely, it the filamentary configuration dissipates, the conditions necessary for the emergence of such stars may become less favorable.

Environmental Factors and Star Formation

"This research underscores the importance of environmental factors-especially the presence of heavy elements-in maintaining filamentary structures, which may be instrumental in planetary system formation," Tokuda states.

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DA362 multiwavelength study insights

Exploring DA 362: Study Unveils More About Compact Symmetric Objects

Introduction to DA 362 and Compact Symmetric Objects (CSOs)

Indian researchers conducted a comprehensive multiwavelength investigation of DA 362, a gamma-ray-emitting compact symmetric object. Findings, detailed in a December 17 arXiv preprint, offer valuable insights into this mysterious phenomenon.

What Are Compact Symmetric Objects (CSOs)?

Compact symmetric objects (CSOs) are young jetted active galactic nuclei (AGN) with projected sizes under 3,300 light-years. While their characteristics remain insufficiently explored, observations reveal symmetric radio morphologies, suggesting these objects are in their early evolutionary stages, with kinematic ages of only a few thousand years. Notably, gamma-ray emissions have been detected from just four CSOs so far.

Introduction to DA 362: A Newly Identified Gamma-Ray Emitting CSO

The most recently identified gamma-ray-emitting compact symmetric object (CSO) is DA 362, also referred to as B2 1413+34. Initially, it was categorized as a blazar condidate of uncertain classification, linked to the gamma-ray source 4FGLJ1416.0+3443.

Multiwavelength Study of DA 362

Astronomers, led by Subhashree Swain from the Inter-University Center for Astronomy and Astrophysics in Pune, India, recently conducted a long-term multiwavelength analysis of DA 362 using data from NASA's Fermi Large Area Telescope (LAT) and Swift satellite. This investigation provided new insights into the nature of this compact symmetric object (CSO).

Key Findings from the Multiwavelength Analysis

"In our investigation, we analyzed the multiwavelength properties of DA 362, a CSO newly recognized as a gamma-ray source by Fermi-LAT, marking it as only the fourth gamma-ray-detected AGN of this type," the authors stated.

Verification of the Gamma-Ray Source Link

The analysis of LAT data verified the link between the gamma-ray source 4FGLJ1416.0+3443 and DA 362. The refined gamma-ray position aligned with the radio source with the 95% confidence interval for gamma-ray uncertainty.

Gamma-Ray Light Curve and Activity

Analysis of the gamma-ray light curve of DA 362 indicates that the source remained predominantly inactive during the first 12 years of LAT observations (2008-2020). However, episodes of flaring activity suggest that the gamma-ray emission likely originates from its core or jet, rather than the radio lobes.

Radio Emissions and Jet Characteristics

In addition, the research identified small, parsec-scale bipolar radio emissions from DA 362 and determined its jet separation velocity to be subluminal. These results establish DA 362 as a bonafide compact symmetric object.

Spectral Properties and Comparison with Other Gamma-Ray Emitting CSOs

By analyzing the gamma-ray spectral properties relative to the three other identified gamma-ray-emitting CSOs, astronomers concluded that DA 362 stands out as the brightest and exhibits a steeper spectrum.

Optical Spectrum and Dust Obscuration

Nevertheless, it was found that DA 362 is exceptionally faint in the optical spectrum, implying potential dust obscuration.

Future Observations and Researcher Directions

The paper's authors suggest that more in-depth observations using advanced facilities are necessary to investigate the broadband physical properties of this CSO and gain further insight into the source of its gamma-ray emission.

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fractal universe cosmic structure mandelbrot

Is the Universe a Fractal? Unraveling the Patterns of Nature

The Cosmic Debate: Is the Universe a Fractal?

For decades, cosmologists have debated whether the universe's large-scale structure exhibits fractal characteristics—appearing identical across scales. The answer is nuanced: not entirely, but in certain respects, yes. It's a complex matter.

The Vast Universe and Its Hierarchical Structure

Our universe is incredibly vast, comprising approximately 2 trillion galaxies. These galaxies are not distributed randomly but are organized into hierarchical structures. Small groups typically consist of up to a dozen galaxies. Larger clusters contain thousands, while immense superclusters extend for millions of light-years, forming intricate cosmic patterns.

Is this where the story comes to an end?

Benoit Mandelbrot and the Introduction of Fractals

During the mid-20th century, Benoit Mandelbrot introduced fractals to a wider audience. While he did not invent the concept—self-similar patterns had been a focus on mathematicians for centuries—Mandelbrot coined the term and catalyzed its modern study. A fractal is defined by a single mathematical formula that describes its structure at every scale, preserving its shape regardless of how much it is magnified or reduced.

The Concept of Fractals in Nature

Fractals are ubiquitous in nature, evident in the branching patterns of trees and the intricate edges of snowflakes. Mandelbrot himself speculated whether the universe might exhibit fractal properties, with similar structures recurring at progressively larger scales as we zoom out.

The Hierarchical Universe: A Fractal-like Pattern?

In some sense, the universe does exhibit a hierarchy of structures across increasingly larger scales. However, this hierarchy has limit. Beyond approximately 300 million light-years, the cosmos transitions to homogeneity, with no larger structures present and appearing uniform at that scale.

Fractal-Like Characteristics in the Cosmic Web

While the universe as a whole is not a fractal, certain aspects of the cosmic web exhibit intriguing fractal-like characteristics. For instance, dark matter 'halos,' which host galaxies and clusters, create nested structures with sub-halos and sub-sub-halos embedded within.

The Voids and Subtle Fractal Patterns

Contrary to popular belief, the voids in our universe are not completely empty. They host faint dwarf galaxies, which align in a delicate, ghostly version of the cosmic web. Simulations reveal that even the sub-voids within these regions contain their own subtle cosmic web structure.

Conclusion: The Persistence of Fractal-Like Patterns

Although the universe isn't a fractal and Mandelbrot's hypothesis doesn't hold true, fractal-like patterns are still pervasive in many places we observe.

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alma dusty planet formation

ALMA Captures Stunning Images of Dusty Planet Formation Site

Introduction to ALMA's Groundbreaking Observations

The Atacama Large Millimeter/submillimeter Array (ALMA) has effectively captured a planet formation site, identifying a dense accumulation of dust grains—essential building blocks for planets—beyond the orbits of nascent planets.

Research Team and Methodology

The international research team, led by Kiyoaki Doi, a former Ph.D. student at the National Astronomical Observatory of Japan (NAOJ) and SOKENDAI, currently a postdoctoral fellow at the Max Planck Institute for Astronomy, conducted high-resolution ALMA observations of the protoplanetary disk surrounding the young star PDS 70 at a wavelength of 3 mm.

Discovering Dust Accumulation Beyond Planetary Orbits

The object contains two known planets, and the latest ALMA observations have uncovered a concentrated accumulation of dust grains beyond their orbits. This discovery implies that the already-formed planets gather material essential for planet formation, possibly aiding in the creation of additional planets. This research enhances our understanding of the formation processes of planetary systems, such as our own solar system, that contain multiple planets.

Significance of the Research

Advancing Our Understanding of Planetary System Formation

Astrophysical Journal Letter has accepted the article, 'Asymmetric Dust Accumulation of the PDS 70 Disk Revealed by ALMA Band 3 Observations,' for publication, and it is available on the arXiv preprint server.

The Role of Dust Grains in Planet Formation

To date, astronomers have identified over 5,000 planets within and beyond our solar system, some of which form multi-planetary systems. These planets are thought to originate from micron-sized dust grains within the protoplanetary disks surrounding young stars. However, the mechanisms driving local dust grain accumulation and their role in forming planetary systems remain poorly understood.

PDS 70: Unique Celestial Body

Planet Formation Confirmed in PDS 70

PDS 70 is the sole known celestial body hosting fully-formed planets, as confirmed by optical and infrared observations, within its protoplanetary disk. Investigating the dust grain distribution in this system will shed light on the interaction between the formed planets and their surrounding disk, as well as their potential role in driving further planet formation.

Earlier ALMA Observations and Limitations

Earlier ALMA observations at a wavelength of 0.87 mm detected ring-like emissions from dust grains located beyond the planetary orbits. However, these emissions may be optically thick, with foreground dust obscuring background grains, potentially leading to an inaccurate representation of the true dust grain distribution.

New ALMA Observations and Findings

High-Resolution 3 mm Observations

Under the leadership of Kiyoaki Doi, the researchers utilized ALMA to conduct high-resolution observations of the protoplanetary disk surrounding PDS 70 at a wavelength of 3 mm. Observations at this wavelength, being optically thinner, offer a more accurate representation of the dust grain distribution.

Distinct Dust Distribution Revealed

The 3 mm observations revealed a distribution distinct from the earlier 0.87 mm data, showing that dust emissions are concentrated in a specific direction within the dust ring beyond the planets. This indicates that planet-forming dust grains accumulate within a localized region, forming a clump.

The Role of Existing Planets in Dust Accumulation

The dust clump observed outside the planets suggests that interactions between the existing planets and the surrounding disk focus dust grains at the outer edge of their orbits. These grains may eventually coalesce into a new planet.

Insights into Planetary System Formation

Planet Formation Process

Planetary system formation, including that of the solar system, can be understood as a sequential  process in which planets form the inside out through repeated interactions. This study provides observational evidence of how existing planets influence their environment and initiate the formation of subsequent planets, advancing our understanding of planetary system development.

Multi-Wavelength Observations for Deeper Insights

According to Kiyoaki Doi, who spearheaded the research, "A celestial body consists of diverse components, each radiating energy at specific wavelengths. Observing it across various wavelengths offers unparalleled insights into its nature."

In PDS 70, planets were identified using optical and infrared wavelengths, while millimeter wavelengths revealed the structure of the protoplanetary disk. This study highlights the disk's varying morphologies across ALMA's observational wavelength range.

Conclusion

The importance of conducting observations across a range of wavelengths, including multi-wavelength studies with ALMA, is evident. To fully comprehend a system, it is essential to observe its various components using a variety of telescope and observational configurations.

Source

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