A detailed observation by Telescópio Espacial James Webb has provided the first direct evidence of how crystalline silicates, minerals that require high temperatures to form, are transported to the cold regions of forming star systems. The data, focused on the protostar EC 53, located approximately 1,300 light-years from Terra, solves an old astronomical puzzle about the presence of these crystals in comets, which originate in icy areas of space.
The protostar, located at Nebulosa of Serpens, was monitored during its activity cycles, revealing that powerful jets and stellar winds, generated during peaks of matter accretion, are responsible for ejecting the newly formed silicates. Esses crystals are created in the hot, inner part of the disk of dust and gas that surrounds the young star, at temperatures exceeding 900 Kelvin.
Previously, the presence of these minerals in celestial bodies such as the comets of Cinturão of Kuiper and Nuvem of The discovery of Webb demonstrates that an active transport mechanism distributes these fundamental components for the formation of rocky planets throughout the protoplanetary system, enriching the material that will give rise to future planets and comets.
Detailed observations with the MIRI instrument
The success of the research depended on the capacity of the Mid-Infrared Instrument (MIRI), one of the main equipment on board the James Webb. MIRI is designed to capture light in the mid-infrared spectrum, which allows astronomers to analyze the chemical composition of cold, distant cosmic objects. Utilizando spectroscopy, the instrument broke down the light coming from EC 53, identifying the specific chemical “signatures” of crystalline silicates in the dust around the star. Essa technique works in a similar way to a barcode, where each element or compound absorbs and emits light at unique wavelengths.
The observations were strategically carried out in two distinct phases of the protostar’s activity cycle: a period of calm and another during a “burst” or outbreak of accretion. Comparing the data collected in these two phases was crucial to mapping the dynamic changes in the disk. The spectra confirmed that crystalline silicates form exclusively in the inner, scorching zone of the disk, a region analogous to the Earth’s orbit in our Sistema Solar, and that the winds generated during the flares act as an efficient transport mechanism, launching the particles to the edges of the system.
Activity cycle of the protostar EC 53
Protostar EC 53 is no ordinary star; it exhibits cyclical and predictable behavior, which makes it an ideal natural laboratory for studying star formation processes. Every 18 months, the star undergoes a burst of accretion that lasts about 100 days. During this period, its luminosity increases dramatically as it consumes gas and dust from its surrounding disk at an accelerating rate.
This intense “feeding” process is the engine behind material ejection. The energy released during the flare generates high-speed polar jets and slower, broader winds that originate from the surface of the inner disk. São these slower winds that carry the newly formed crystalline silicates with them, as if they were a cosmic conveyor belt.
The regularity of these events allowed the international team of researchers to time their observations with James Webb to capture the system at key moments, gaining an unprecedented view of the complete cycle of formation and transport of these minerals essential to the composition of rocky planets.
Types of silicates identified
Spectral analyzes performed by the MIRI instrument not only confirmed the presence of crystalline silicates, but also identified their composition with remarkable accuracy. Entre the minerals detected are forsterite and enstatite, both common on our own planet and in bodies on Sistema Solar. Forsterite is a magnesium-rich silicate, a key component of igneous and metamorphic rocks in Terra, such as peridotite found in the Earth’s mantle. Já enstatite is another silicate mineral often found in meteorites, indicating that the processes observed in EC 53 are analogous to those that occurred in the early days of our own planetary system. Essas particles, smaller than a grain of sand, are the fundamental building blocks that, over millions of years, coalesce to form planetesimals and, eventually, rocky planets like Terra, Marte and Vênus. The detection of these specific compounds reinforces theoretical models of planet formation and establishes a direct connection between the chemistry of young disks and the geology of mature planets.
Disk transport mechanism
The James Webb data allowed us to create a clear visual model of how silicates travel from the hot center to the icy periphery of EC 53’s protoplanetary disk. The process begins in the inner region, where temperatures are high enough to crystallize amorphous silicate dust.
When the protostar enters its accretion phase, the intense activity generates winds and jets that depart from this central region. Crystalline silicate particles are picked up by these flows of matter and launched upward and outward, following a ballistic trajectory.
This “cosmic highway” transports the crystals to the cold edges of the disk, an area where temperatures are low enough for gases like water and carbon dioxide to freeze. Lá, silicates can mix with ice grains and incorporate into forming bodies, such as asteroids and comets.
This mechanism elegantly explains how materials processed at high temperatures end up in celestial bodies that were formed and have always existed in extreme cold environments, solving one of the biggest questions in planetary science.
Context in Nebulosa of Serpens
Protostar EC 53 is not isolated in space; it is part of Nebulosa of Serpens, a vast cloud of gas and dust that is one of the closest star-forming regions to Terra. Localizada 1,300 light years away, this nebula functions as a stellar nursery, housing thousands of young stars at different stages of development.
This environment rich in raw materials is fundamental for studying the birth of stars and planets. Because it is still enveloped in a dense cocoon of gas and dust, EC 53 and its disk are invisible in visible light wavelengths. Somente infrared telescopes like the James Webb can penetrate this dust curtain and reveal the processes taking place inside.
Instruments used in observations
Complete understanding of the EC 53 system was achieved through the combination of multiple instruments onboard James Webb. Enquanto MIRI provided the crucial spectral data for the chemical analysis, the Near-Infrared Camera (NIRCam) was used to capture detailed images of the system’s structure.
NIRCam images, obtained in 2024, revealed the morphology of the winds and jets emanating from the protostar. In Nessas images, it is possible to see the light from the central star reflected by the disk’s dust and the cone- and arc-shaped structures created by the outflows. Combining NIRCam’s wide-field view with MIRI’s precise chemical analysis allowed scientists to correlate the presence of the silicates with the ejection structures, confirming that winds were indeed the transport mechanism.
International team and publishing
The research was conducted by an international team of astronomers led by Jeong-Eun Lee, of Universidade Nacional of The study, which included the collaboration of scientists from renowned institutions such as Conselho Nacional of Pesquisa of Canadá and Space Telescope Science Institute of Estados Unidos, was published in the prestigious scientific journal
Future evolution of the system
The EC 53 system is just at the beginning of its evolutionary journey, which will unfold over millions of years. Constant collisions between dust grains, crystalline silicates and boulders in the disk will continue to build larger and larger bodies. Esse processo de aglutinação gradual é o caminho que leva à formação de planetas rochosos no interior do sistema e, possivelmente, de gigantes gasosos ou gelados nas regiões mais externas, dependendo da quantidade de material disponível.
Over time, most of the disk’s gas and dust will be incorporated into new planets or dissipated by radiation from the central star, which will evolve to become a stable star, similar to our Sol. The end result will be a mature planetary system, where the crystalline silicates, originally forged at the heart of the system, will be distributed everywhere, from the surfaces of rocky planets to the icy cores of comets in their most distant orbits.