Month: June 2024

  • NASA Simulation Reveals Origins of Asteroid Belt’s Vesta-like Objects.

     

    NASA-supported researchers have conducted a groundbreaking study using simulations to delve into the origins of objects in the asteroid belt, shedding light on their formation and evolution. The study, detailed in The Planetary Science Journal, focuses on understanding the composition and distribution of S- and C-complex objects within the belt.


    The research team, led by Rogerio Deienno from the Southwest Research Institute in Boulder, Colorado, utilized data from NASA’s Dawn spacecraft, which extensively explored Vesta, the second most massive object in the asteroid belt after Ceres. Vesta, with a composition akin to S-complex objects, provides a key constraint for the simulations.


    The simulations revealed insights into the early dynamics of the asteroid belt, suggesting that its total mass during the solar system’s formation was significantly lower than previously estimated. Specifically, the team found that if the initial mass of the asteroid belt had been larger, there would be more Vesta-sized objects present today. However, the current distribution indicates a relatively low initial mass—approximately five times less than the mass of the Moon.


    Moreover, the study suggests that objects like Vesta likely didn’t form directly within the main asteroid belt but originated elsewhere in the solar system before migrating to their current locations. This migration process highlights the dynamic history of our solar system’s formation and the intricate pathways taken by celestial bodies over billions of years.


    The findings underscore the importance of simulations in reconstructing the early solar system’s conditions and the ongoing evolution of planetary bodies. By refining our understanding of how and where objects like Vesta formed, researchers gain deeper insights into the broader processes that shaped our solar system into its current configuration.

  • NASA’s Juno Mission Provides Close-Up View of Lava Lakes on Jupiter’s Moon Io.

     

    On February 3, NASA’s Juno spacecraft, equipped with the JunoCam instrument, captured a striking image of two volcanic plumes ascending above the horizon of Jupiter’s moon Io. Taken from a distance of approximately 2,400 miles (3,800 kilometers), this snapshot offers a close-up view of the active geological processes shaping Io’s rugged surface.

    Infrared imagery from NASA’s Juno probe is shedding new light on Io, Jupiter’s most volcanic moon. Recent discoveries reveal the extensive distribution of lava lakes across Io’s surface, offering unprecedented insights into its volcanic activity. Juno’s Jovian Infrared Auroral Mapper (JIRAM), provided by the Italian Space Agency, played a crucial role in capturing these findings by detecting infrared signatures. Published in Nature Communications Earth and Environment on June 20, the research marks a significant step forward in understanding the geological processes at work on Io.


    Io has fascinated astronomers since its discovery in 1610 by Galileo Galilei, revealing a moon slightly larger than Earth’s Moon. Nearly 369 years later, NASA’s Voyager 1 spacecraft captured the first volcanic eruption on Io. Subsequent missions to Jupiter, featuring multiple Io flybys, unveiled additional volcanic plumes and vast lava lakes. Scientists now regard Io, influenced by gravitational tugs from nearby moons and Jupiter, as the most volcanically active body in our solar system. Despite numerous theories on Io’s volcanic eruptions, there remains a scarcity of supporting data.


    During flybys in May and October 2023, NASA’s Juno spacecraft approached Io at distances of approximately 21,700 miles (35,000 kilometers) and 8,100 miles (13,000 kilometers), respectively. Juno’s instruments, including the Jovian Infrared Auroral Mapper (JIRAM), provided detailed observations of Io’s complex terrain and volcanic activity, enriching our understanding of this enigmatic moon.


    Infrared data collected on October 15, 2023, by NASA’s Juno Infrared Auroral Mapper (JIRAM) instrument reveals Chors Patera, a prominent lava lake on Jupiter’s moon Io. Analysis by the mission team suggests that the lake is predominantly covered by a thick, molten crust, with a distinct hot ring encircling its edges where molten lava from Io’s interior is directly exposed to space.


    JIRAM, designed to capture infrared light invisible to the human eye emanating from deep within Jupiter, delves into the gas giant’s atmosphere down to 30 to 45 miles beneath its cloud tops. During Juno’s extended mission, the instrument has expanded its scope to include Io, Europa, Ganymede, and Callisto. Particularly striking are JIRAM’s images of Io, revealing bright rings encircling hot spot floors.Alessandro Mura, a Juno co-investigator from the National Institute for Astrophysics in Rome, highlighted the instrument’s high spatial resolution, coupled with Juno’s advantageous flyby positions, uncovering Io’s entire surface adorned with lava lakes nestled in caldera-like formations. Mura estimates that approximately 3% of Io’s surface features these molten lava reservoirs, formed within depressions created by volcanic eruptions and collapses known as calderas.


    In the realm of Io’s volcanic activity, JIRAM’s recent flyby has unveiled intriguing insights into the moon’s fiery landscapes. The data not only underscores Io’s vast reservoirs of lava but also offers a peek into its subsurface dynamics. Infrared imagery of multiple lava lakes on Io reveals a distinctive pattern: a narrow band of molten lava encircling the lake’s perimeter, separating the central crust from the lake’s enclosing walls. 


    This phenomenon suggests a continuous recycling process where molten material erupts into the lava lakes and is subsequently reintegrated into Io’s subsurface, without significant outward lava flows beyond the lake rims. This delicate balance hints at a complex system of magma circulation beneath Io’s turbulent surface, perpetuating its reputation as a “fire-breathing” moon of the Solar System.


    “We now understand that the predominant volcanic activity on Io involves vast lava lakes where magma cycles up and down,” explained Mura. These lava lakes exhibit a distinct lava ring around their perimeters, akin to those observed in Hawaiian lava lakes, formed as the molten crust collides with the lake walls. These walls likely tower hundreds of meters high, preventing magma from spilling out of the bowl-shaped paterae and spreading across Io’s surface. JIRAM data indicates that these hot spots are mostly covered by a rocky crust that moves cyclically due to magma upwelling at the center. This crust interacts with the lake walls, causing deformation and occasional breaks that expose the molten lava below.


    An alternative hypothesis proposes that magma wells up at the lake’s center, spreading outward and forming a sinking crust along the rim, thereby exposing lava. Scott Bolton, principal investigator for Juno at the Southwest Research Institute, emphasized the significance of recent JIRAM observations from close Io flybys in late 2023 and early 2024. These findings are shedding new light on Io’s volcanic processes, complementing Juno’s ongoing efforts to map the volcanoes at Io’s poles. With Juno’s 62nd flyby of Jupiter, which included an Io pass at 18,175 miles (29,250 kilometers) altitude on June 13, and the upcoming 63rd flyby scheduled for July 16, JIRAM continues to prove invaluable in unraveling the mysteries of this geologically dynamic moon.

  • Hubble Captures an Image of Nebula RCW 7, Revealing Massive Protostars in Constellation Puppis.

     

    A visually striking collection of interstellar gas and dust is captured in this latest image from the NASA/ESA Hubble Space Telescope. Named RCW 7, this nebula is located over 5,300 light-years away in the constellation Puppis.


    Nebulae, such as RCW 7, are rich in the raw materials needed to form new stars. Under the influence of gravity, parts of these molecular clouds collapse, coalescing into very young, developing stars known as protostars. These protostars remain surrounded by spinning discs of leftover gas and dust. In RCW 7, the forming protostars are particularly massive, emitting strong ionizing radiation and fierce stellar winds that transform the nebula into an H II region.


    H II regions are characterized by hydrogen ions; H I denotes a normal hydrogen atom, whereas H II is hydrogen that has lost its electron, becoming an ion. Ultraviolet radiation from the massive protostars excites the hydrogen in the nebula, causing it to emit light, resulting in the nebula’s soft pinkish glow.


    The Hubble data for this image were collected from a study of a particularly massive protostellar binary named IRAS 07299-1651. This binary is still cocooned in gas within the curling clouds toward the top of the image. To expose this star and its siblings, astronomers utilized Hubble’s Wide Field Camera 3 in near-infrared light. While the massive protostars are brightest in ultraviolet light, they emit substantial infrared light as well. Infrared light’s longer wavelength allows it to penetrate much of the gas and dust, enabling Hubble to capture this stunning image. Many of the larger stars seen in the image are actually foreground stars, positioned between the nebula and our solar system, and are not part of the nebula.


    The formation of an H II region signals the beginning of the end for a molecular cloud like RCW 7. Within a few million years, radiation and winds from the massive stars will gradually disperse the nebula’s gas. This process will be accelerated by supernova explosions as the most massive stars reach the end of their lives. New stars in this nebula will incorporate only a fraction of its gas, with the remainder spreading throughout the galaxy to eventually form new molecular clouds.

  • NASA’s Hubble Space Telescope Captures New Image of Galaxy NGC 1546 in Alternate Operating Mode.

     

    NASA’s Hubble Space Telescope has successfully resumed operations and captured its first new images after switching to an alternate operating mode that uses one gyroscope (gyro). The spacecraft returned to science operations on June 14, following several weeks offline due to an issue with one of its gyros, which are essential for controlling and orienting the telescope.


    The newly captured image showcases NGC 1546, a nearby galaxy located in the constellation Dorado. The galaxy’s orientation offers a striking view of its dust lanes, which are illuminated and backlit by the core of the galaxy. The dust absorbs light from the core, giving it a rusty-brown hue, while the core itself shines brightly with a yellowish light indicative of an older star population. Regions of active star formation, characterized by a brilliant blue color, are visible through the dust. Additionally, several background galaxies can be seen, including an edge-on spiral just to the left of NGC 1546.


    Hubble’s Wide Field Camera 3 captured this image as part of a collaborative observing program with NASA’s James Webb Space Telescope. This program also incorporates data from the Atacama Large Millimeter/submillimeter Array (ALMA), providing scientists with a highly detailed, multiwavelength view of star formation and evolution.


    This image is one of the first observations taken with Hubble since transitioning to the new pointing mode, which promises more stable and consistent science operations. NASA expects that Hubble can conduct most of its science observations in this mode, continuing its groundbreaking study of the cosmos.


    Hubble’s new image of a spectacular galaxy demonstrates the full success of our new, more stable pointing mode for the telescope,” said Dr. Jennifer Wiseman, senior project scientist for Hubble at NASA’s Goddard Space Flight Center in Greenbelt, Maryland. “We’re poised now for many years of discovery ahead, and we’ll be looking at everything from our solar system to exoplanets to distant galaxies. Hubble plays a powerful role in NASA’s astronomical toolkit.

  • Webb and ALMA Unveil Hidden Secrets of the WL 20 Star System in Rho Ophiuchi.

     

    Managed by NASA’s Jet Propulsion Laboratory through launch, Webb’s Mid-Infrared Instrument (MIRI) recently unveiled a significant discovery. Scientists were astonished when NASA’s James Webb Space Telescope focused on a group of young stars known as WL 20. Despite being studied since the 1970s with at least five other telescopes, it was Webb’s unparalleled resolution and specialized instruments that revealed WL 20S to be a binary star system, formed about 2 million to 4 million years ago.


    This discovery, using Webb’s MIRI, was announced at the 244th meeting of the American Astronomical Society on June 12. MIRI not only identified the twin stars but also detected matching jets of gas streaming from their north and south poles. “Our jaws dropped,” said Mary Barsony, lead author of the study. “We thought we knew this source well, but MIRI’s capabilities showed us otherwise. It’s like having brand new eyes.”


    Further observations by the Atacama Large Millimeter/submillimeter Array (ALMA) in Chile revealed disks of dust and gas around both stars, suggesting possible planet formation. These findings indicate the stars are transitioning from their early developmental stage, offering scientists a rare chance to study their evolution into maturity.


    “The power of these two telescopes together is really incredible,” said Mike Ressler, MIRI project scientist at NASA’s Jet Propulsion Laboratory and co-author of the study. “Seeing these as two stars instead of one changes our interpretation of the ALMA data, which now shows two distinct disks. This provides new insights into the stars’ critical developmental phase.”


    This artist’s concept depicts two young stars nearing the end of their formation, encircled by gas and dust disks from which planets may form, with jets of gas shooting from their poles.


    Stellar Jets : A Star-Forming Region Revealed by Webb.


    This image of the WL 20 star group combines ALMA and Webb’s MIRI data, showing blue and green gas jets from twin stars’ poles and pink disks of dust and gas surrounding them.


    WL 20 resides in a much larger, well-studied star-forming region of the Milky Way galaxy called Rho Ophiuchi. This massive cloud of gas and dust, about 400 light-years from Earth, obscures the view of the stars within at visible wavelengths. However, the James Webb Space Telescope (Webb) with its infrared capabilities can pierce through these dusty veils.


    Webb’s Mid-Infrared Instrument (MIRI) detects the longest infrared wavelengths of any instrument on the telescope. This allows it to peer into obscured regions like WL 20, revealing details that were previously hidden. While radio waves can also penetrate dust, they don’t always provide the same level of detail as infrared light.


    The key to unlocking the true nature of WL 20 came from the combination of Webb’s observations and those from another powerful instrument, the Atacama Large Millimeter/submillimeter Array (ALMA). ALMA observed the disks of gas and dust surrounding the stars in WL 20S emitting light in the submillimeter range, which also penetrates the dust clouds. However, these observations could have been misinterpreted as a single disk with a gap.


    Here’s where MIRI played a crucial role. The stellar jets emanating from the stars, composed of charged particles, radiate in mid-infrared wavelengths detectable by MIRI but not at submillimeter wavelengths observed by ALMA. Only an instrument with MIRI’s combined spatial and spectral resolution could definitively reveal these jets, providing the crucial evidence that WL 20S is actually a binary star system.


    ALMA Observations and Stellar Formation Phases.



    ALMA (Atacama Large Millimeter/submillimeter Array) plays a crucial role in our understanding of star formation. By observing clouds of leftover material around young stars, ALMA provides insights into their evolution. These clouds, composed of whole molecules like carbon monoxide, emit light at longer wavelengths. Interestingly, ALMA’s observations reveal the absence of such clouds, indicating that the stars have progressed beyond their initial formation phase. The scientific community eagerly awaits further revelations from the James Webb Space Telescope (Webb), which promises to unlock more secrets about the life cycle of stars. 


    Webb, an international collaboration led by NASA, ESA, and CSA, is poised to explore our solar system, distant exoplanets, and the enigmatic structures of the universe. The Mid-Infrared Instrument (MIRI), developed through a partnership between NASA and ESA, will be a key player in this cosmic exploration. George Rieke (University of Arizona) leads the MIRI science team, while Gillian Wright oversees the European contributions. The MIRI cryocooler development involved collaboration between JPL, Northrop Grumman, and NASA’s Goddard Space Flight Center.

  • James Webb Space Telescope Unlocks New Insights into the Crab Nebula.

     

    This image by NASA’s James Webb Space Telescope’s NIRCam (Near-Infrared Camera) and MIRI (Mid-Infrared Instrument) shows different structural details of the Crab Nebula. The supernova remnant comprises several components, including doubly ionized sulfur (green), warm dust (magenta), and synchrotron emission (blue). Yellow-white mottled filaments within the Crab’s interior represent areas where dust and doubly ionized sulfur coincide. The observations were taken as part of General Observer program 1714.

    A team of scientists utilized NASA’s James Webb Space Telescope to investigate the Crab Nebula, a supernova remnant located 6,500 light-years away in the constellation Taurus. By employing the telescope’s MIRI (Mid-Infrared Instrument) and NIRCam (Near-Infrared Camera), the team is shedding new light on the complex history of this celestial phenomenon.


    A Supernova from the Past.


    The Crab Nebula is the result of a core-collapse supernova, which marks the violent death of a massive star. This explosion was observed on Earth in 1054 CE and was visible even during the daytime. Today, the remnants form an expanding shell of gas and dust driven by a pulsar—a rapidly spinning and highly magnetized neutron star.


    Unraveling a Cosmic Mystery.


    The Crab Nebula’s atypical composition and low explosion energy were previously attributed to an electron-capture supernova. This rare type of explosion occurs when a star’s core, primarily composed of oxygen, neon, and magnesium, collapses. However, new data from the Webb Telescope suggest alternative explanations. 


    “Now the Webb data widen the possible interpretations,” said Tea Temim, lead author of the study at Princeton University. “The composition of the gas no longer requires an electron-capture explosion but could also be explained by a weak iron core-collapse supernova.”


    Revisiting Past Calculations.

    Previous research estimated the total kinetic energy of the explosion by analyzing the present-day ejecta’s quantity and velocity. These studies concluded that the explosion was relatively low-energy and involved a progenitor star with a mass between eight to ten solar masses. This is a borderline case between stars that end in supernovae and those that do not.


    Yet, discrepancies remain between the electron-capture supernova theory and observed data, such as the rapid motion of the Crab Nebula’s pulsar. Recent advances in understanding iron core-collapse supernovae indicate that these can also result in low-energy explosions if the star’s mass is sufficiently low.


    Webb’s Spectroscopic Capabilities.


    To address these uncertainties, Temim’s team used Webb’s spectroscopic tools to examine two specific areas within the Crab’s inner filaments. They focused on the nickel to iron (Ni/Fe) abundance ratio, which differs in electron-capture supernovae compared to other types. Earlier measurements suggested a high Ni/Fe ratio, supporting the electron-capture scenario.


    Webb’s precise infrared spectrometry provided a more accurate Ni/Fe ratio. The results indicated an elevated but lower ratio than previous estimates, aligning with both electron-capture and low-mass iron core-collapse supernova models. 


    Mapping the Nebula.


    In addition to spectral data, the Webb Telescope observed the broader environment of the Crab Nebula, analyzing synchrotron emission and dust distribution. MIRI’s imaging capabilities allowed the team to isolate and map the warm dust emission in unprecedented detail. The outer filaments contain warmer dust, while cooler grains are concentrated near the center.


    “Where dust is seen in the Crab is interesting because it differs from other supernova remnants,” noted Nathan Smith of the Steward Observatory. “In those objects, the dust is in the very center. In the Crab, the dust is found in the dense filaments of the outer shell. The Crab Nebula lives up to a tradition in astronomy: The nearest, brightest, and best-studied objects tend to be bizarre.”


    ### Future Directions


    This study represents a significant step in understanding the Crab Nebula’s complex history. However, further observations and theoretical work are needed to conclusively determine the nature of the explosion that created it. Expanding the spectral analysis to more regions within the nebula and identifying additional elements could provide deeper insights into its origins.

  • NASA/ESA Hubble Space Telescope Reveals Peculiar Globular Cluster in Large Magellanic Cloud.

     

    This NASA/ESA Hubble Space Telescope image features the globular cluster NGC 2005. Located about 750 light-years from the center of the Large Magellanic Cloud (LMC), this cluster provides unique insights into galaxy evolution and the history of our universe.

    The Hubble Space Telescope, a joint project of NASA and the European Space Agency (ESA), has captured a striking image of the globular cluster NGC 2005. Located approximately 750 light-years from the center of the Large Magellanic Cloud (LMC), this cluster stands out due to its unique properties in comparison to its surrounding environment. The LMC itself is the Milky Way’s largest satellite galaxy, situated around 162,000 light-years from Earth.


    Globular clusters are densely packed collections of stars, often containing tens of thousands or even millions of stars. The intense gravitational forces within these clusters ensure their stability, allowing them to exist for billions of years. As such, they often consist of very old stars, making them invaluable for studying the early universe. Much like fossils provide clues about ancient life on Earth, globular clusters reveal important details about the characteristics of ancient stars.


    Current theories on galaxy evolution propose that larger galaxies form through the merging of smaller ones. If true, this would mean that the oldest stars in nearby galaxies originated from different galactic environments. Due to their ancient and stable nature, globular clusters like NGC 2005 are excellent subjects for testing these theories.


    What makes NGC 2005 particularly intriguing is its chemical composition, which differs significantly from the surrounding stars in the LMC. This anomaly suggests that the LMC experienced a merger with another galaxy in its distant past. While the other galaxy has since merged and dispersed, NGC 2005 remains as an ancient relic, providing evidence of this long-ago cosmic event.


    The study of NGC 2005 and similar globular clusters helps astronomers piece together the complex history of galaxy formation and evolution, offering insights into the dynamic processes that shaped the universe as we see it today.

  • In 1993, Hubble revealed an abundant planet-forming disk in the Orion Nebula.

    A NASA Hubble Space Telescope image of a region of the Great Nebula in Orion, one of the closest areas of recent star formation, offers a glimpse into cosmic creation. The nebula, a vast gas cloud 1,500 light-years away, is illuminated by young, hot stars. Many fainter stars are encircled by dust and gas disks, slightly over twice the Solar System’s diameter. A plume of gas in the upper left reveals material ejected from a newly formed star. The image, taken on December 29, 1993, spans 1.6 light-years and uses color to depict emissions: red for Nitrogen, green for Hydrogen, and blue for Oxygen.

    In 1993 — Observations with the Hubble Space Telescope have provided the most compelling evidence yet that planet formation is a common occurrence in our galaxy. A team led by Dr. C. Robert O’Dell of Rice University has uncovered clear indications that disks of dust, the essential material for planet formation, are present around many stars in the Orion Nebula, a prominent star-forming region located about 1,500 light-years from Earth.

    Dr. O’Dell, along with Zheng Wen, formerly of Rice University and now at the University of Kentucky, examined 110 stars in the Orion Nebula and identified dust disks around 56 of them. These disks, termed “proplyds” by O’Dell, were initially discovered in 1992 through Hubble images. More detailed observations confirm that these structures are indeed pancake-shaped disks rather than dust shells, strengthening the theory that they are the precursors to planetary systems.

    These disks are composed of carbon, silicates, and other materials similar to those that formed the planets in our solar system about 4.5 billion years ago. While current technology makes it easier to detect the stars than the disks, O’Dell suggests that many more stars likely have such protoplanetary material. He has even measured portions of the mass of these disks, finding they contain enough material to form Earth-like planets.

    The only confirmed planetary system known to date comprises three Earth-sized planets orbiting a neutron star, an atypical example as these planets likely formed after a stellar explosion. The findings in the Orion Nebula, however, suggest that planet-forming disks are abundant in young star clusters, implying that planetary systems like our own might be widespread in the universe.

    This revelation holds significant implications for the search for extraterrestrial life. Planets are essential for life as we know it, offering the necessary conditions and materials. The widespread presence of planet-forming disks increases the probability that planets, and possibly life, are common in the universe.

    Moreover, the Hubble images have resolved young stars at the center of each disk, showing that stars with masses comparable to or smaller than our Sun are likely to possess these disks. Stars hotter than our Sun may destroy their dust disks before planets can form, but the majority of stars in regions like Orion could potentially host planets.

    One of Hubble’s striking images shows a dark elliptical disk silhouetted against the bright background of the Orion Nebula, providing the most direct evidence to date for protoplanetary disks. The resolution of these images has allowed O’Dell to accurately determine the mass of the disks, finding them to be several times the mass of Earth and spanning 53 billion miles across, with the central star being about one-fifth the mass of our Sun.

    These discoveries support long-standing theories about the formation of planetary systems and highlight the significance of circumstellar disks in this process. O’Dell’s findings will be detailed in the November 20 issue of *The Astrophysical Journal*, marking a significant milestone in our understanding of planetary genesis and the potential for life beyond Earth.

  • Researchers Unveil New Framework for Understanding Emergence in Complex System.

     

    Jupiter’s Great Red Spot, seen in this animation based on Voyager 1 and Hubble images, has swirled for hundreds of years, exemplifying how large-scale patterns and organization can arise from innumerable microscopic interactions.

    HA few centuries ago, the swirling polychromatic chaos of Jupiter’s atmosphere spawned the immense vortex that we call the Great Red Spot.


    From the frantic firing of billions of neurons in your brain comes your unique and coherent experience of reading these words.


    As pedestrians each try to weave their path on a crowded sidewalk, they begin to follow one another, forming streams that no one ordained or consciously chose.


    The world is full of such emergent phenomena: large-scale patterns and organization arising from innumerable interactions between component parts. And yet there is no agreed scientific theory to explain emergence. Loosely, the behavior of a complex system might be considered emergent if it can’t be predicted from the properties of the parts alone. But when will such large-scale structures and patterns arise, and what’s the criterion for when a phenomenon is emergent and when it isn’t? Confusion has reigned. “It’s just a muddle,” said Jim Crutchfield, a physicist at the University of California, Davis.


    “Philosophers have long been arguing about emergence, and going round in circles,” said Anil Seth, a neuroscientist at the University of Sussex in England. The problem, according to Seth, is that we haven’t had the right tools — “not only the tools for analysis, but the tools for thinking. Having measures and theories of emergence would not only be something we can throw at data but would also be tools that can help us think about these systems in a richer way.”


    Though the problem remains unsolved, over the past few years, a community of physicists, computer scientists and neuroscientists has been working toward a better understanding. These researchers have developed theoretical tools for identifying when emergence has occurred. And in February, Fernando Rosas, a complex systems scientist at Sussex, together with Seth and five co-authors, went further, with a framework for understanding how emergence arises.


    A complex system exhibits emergence, according to the new framework, by organizing itself into a hierarchy of levels that each operate independently of the details of the lower levels. The researchers suggest we think about emergence as a kind of “software in the natural world.” Just as the software of your laptop runs without having to keep track of all the microscale information about the electrons in the computer circuitry, so emergent phenomena are governed by macroscale rules that seem self-contained, without heed to what the component parts are doing.


    Using a mathematical formalism called computational mechanics, the researchers identified criteria for determining which systems have this kind of hierarchical structure. They tested these criteria on several model systems known to display emergent-type phenomena, including neural networks and Game-of-Life-style cellular automata. Indeed, the degrees of freedom, or independent variables, that capture the behavior of these systems at microscopic and macroscopic scales have precisely the relationship that the theory predicts.


    No new matter or energy appears at the macroscopic level in emergent systems that isn’t there microscopically, of course. Rather, emergent phenomena, from Great Red Spots to conscious thoughts, demand a new language for describing the system. “What these authors have done is to try to formalize that,” said Chris Adami, a complex-systems researcher at Michigan State University. “I fully applaud this idea of making things mathematical.”


    A Need for Closure.


    Rosas came at the topic of emergence from multiple directions. His father was a famous conductor in Chile, where Rosas first studied and played music. “I grew up in concert halls,” he said. Then he switched to philosophy, followed by a degree in pure mathematics, giving him “an overdose of abstractions” that he “cured” with a Ph.D. in electrical engineering.


    A few years ago, Rosas started thinking about the vexed question of whether the brain is a computer. Consider what goes on in your laptop. The software generates predictable and repeatable outputs for a given set of inputs. But if you look at the actual physics of the system, the electrons won’t all follow identical trajectories each time. “It’s a mess,” said Rosas. “It’ll never be exactly the same.”


    The software seems to be “closed,” in the sense that it doesn’t depend on the detailed physics of the microelectronic hardware. The brain behaves somewhat like this too: There’s a consistency to our behaviors even though the neural activity is never identical in any circumstance.


    Rosas and colleagues figured that in fact there are three different types of closure involved in emergent systems. Would the output of your laptop be any more predictable if you invested lots of time and energy in collecting information about all the microstates — electron energies and so forth — in the system? Generally, no. This corresponds to the case of informational closure: As Rosas put it, “All the details below the macro are not helpful for predicting the macro.”


    What if you want not just to predict but to control the system — does the lower-level information help there? Again, typically no: Interventions we make at the macro level, such as changing the software code by typing on the keyboard, are not made more reliable by trying to alter individual electron trajectories. If the lower-level information adds no further control of macro outcomes, the macro level is causally closed: It alone is causing its own future.


    This situation is rather common. Consider, for instance, that we can use macroscopic variables like pressure and viscosity to talk about (and control) fluid flow, and knowing the positions and trajectories of individual molecules doesn’t add useful information for those purposes. And we can describe the market economy by considering companies as single entities, ignoring any details about the individuals that constitute them.


    The existence of a useful coarse-grained description doesn’t, however, by itself define an emergent phenomenon, said Seth. “You want to say something else in terms of the relationship between levels.” Enter the third level of closure that Rosas and colleagues think is needed to complete the conceptual apparatus: computational closure. For this, they have turned to computational mechanics, a discipline pioneered by Crutchfield.


    Crutchfield introduced a conceptual device called the ε- (epsilon) machine. This device can exist in some finite set of states and can predict its own future state on the basis of its current one. It’s a bit like an elevator, said Rosas; an input to the machine, like pressing a button, will cause the machine to transition to a different state (floor) in a deterministic way that depends on its past history — namely, its current floor, whether it’s going up or down and which other buttons were pressed already. Of course, an elevator has myriad component parts, but you don’t need to think about them. Likewise, an ε-machine is an optimal way to represent how unspecified interactions between component parts “compute” — or, one might say, cause — the machine’s future state.


    Computational mechanics allows the web of interactions between a complex system’s components to be reduced to the simplest description, called its causal state. The state of the complex system at any moment, which includes information about its past states, produces a distribution of possible future states. Whenever two or more such present states have the same distribution of possible futures, they are said to be in the same causal state. Our brains will never twice have exactly the same firing pattern of neurons, but there are plenty of circumstances where nevertheless we’ll end up doing the same thing.


    Rosas and colleagues considered a generic complex system as a set of ε-machines working at different scales. One of these might, say, represent all the molecular-scale ions, ion channels and so forth that produce currents in our neurons; another represents the firing patterns of the neurons themselves; another, the activity seen in compartments of the brain such as the hippocampus and frontal cortex. The system (here the brain) evolves at all those levels, and in general the relationship between these ε-machines is complicated. But for an emergent system that is computationally closed, the machines at each level can be constructed by coarse-graining the components on just the level below: They are, in the researchers’ terminology, “strongly lumpable.” We might, for example, imagine lumping all the dynamics of the ions and neurotransmitters moving in and out of a neuron into a representation of whether the neuron fires or not. In principle, one could imagine all kinds of different “lumpings” of this sort, but the system is only computationally closed if the ε-machines that represent them are coarse-grained versions of each other in this way. “There is a nestedness” to the structure, Rosas said.


    A highly compressed description of the system then emerges at the macro level that captures those dynamics of the micro level that matter to the macroscale behavior — filtered, as it were, through the nested web of intermediate ε-machines. In that case, the behavior of the macro level can be predicted as fully as possible using only macroscale information — there is no need to refer to finer-scale information. It is, in other words, fully emergent. The key characteristic of this emergence, the researchers say, is this hierarchical structure of “strongly lumpable causal states.”


    Leaky Emergence.


    The researchers tested their ideas by seeing what they reveal about a range of emergent behaviors in some model systems. One is a version of a random walk, where some agent wanders around haphazardly in a network that could represent, for example, the streets of a city. A city often exhibits a hierarchy of scales, with densely connected streets within neighborhoods and much more sparsely connected streets between neighborhoods. The researchers find that the outcome of a random walk through such a network is highly lumpable. That is, the probability of the wanderer starting in neighborhood A and ending up in neighborhood B — the macroscale behavior — remains the same regardless of which streets within A or B the walker randomly traverses.


    The researchers also considered artificial neural networks like those used in machine-learning and artificial-intelligence algorithms. Some of these networks organize themselves into states that

  • The Unveiling of NGC 4414: A Milestone in Astronomical Observation.

     

    In 1995, the Hubble Space Telescope captured a breathtaking image of the spiral galaxy NGC 4414, marking a significant achievement in the Hubble Space Telescope Key Project on the Extragalactic Distance Scale. This remarkable effort was spearheaded by Dr. Wendy Freedman from the Observatories of the Carnegie Institution of Washington, along with an international team of astronomers who meticulously observed NGC 4414 over 13 different occasions spanning two months.


    The team utilized Hubble’s Wide Field Planetary Camera 2 (WFPC2) to capture images through three distinct color filters. By studying these images and carefully measuring the brightness of variable stars within NGC 4414, the astronomers were able to accurately determine the galaxy’s distance from Earth.


    Their findings revealed that NGC 4414 is situated 19.1 megaparsecs, or approximately 60 million light-years, away. This measurement, along with similar data from nearby galaxies, significantly enhances our understanding of the universe’s rate of expansion. The Hubble constant (H0), a critical value in astronomy, is derived from how quickly galaxies are receding from us relative to their distances. This constant is essential for calculating distances, sizes, intrinsic luminosities of celestial objects, and even the age of the universe itself.


    Due to the substantial size of NGC 4414 compared to the WFPC2 detectors, the 1995 observations only captured half of the galaxy. In 1999, the Hubble Heritage Team revisited NGC 4414 to complete its portrait, using the same filters as before. The result was a magnificent full-color image of the entire dusty spiral galaxy.


    The new image vividly depicts the central regions of NGC 4414, which, like most spiral galaxies, are populated by older, yellow, and red stars. The outer spiral arms, in contrast, shine with a bluish hue due to the ongoing formation of young, blue stars. These bright, young stars stand out individually thanks to Hubble’s high-resolution capabilities. Additionally, the arms are rich in clouds of interstellar dust, appearing as dark patches and streaks silhouetted against the starlight.


    This comprehensive and stunning portrait of NGC 4414 not only exemplifies the power of the Hubble Space Telescope but also represents a crucial step in our quest to understand the vast cosmos.