NASA’s Telescópio Espacial James Webb has obtained conclusive evidence about the formation of crystalline silicates in protoplanetary disks. Observações from the MIRI instrument identified these crystals in the hot inner region around the protostar EC 53, located in Nebulosa of Serpens, about 1,300 light-years from Terra. The data, collected during phases of the star’s activity, shows that powerful outflows transport materials to the cold edges of the disk.
This discovery solves an old enigma about the presence of crystalline silicates in Sistema Solar comets, which inhabit ultracold regions such as Cinturão of Kuiper and Nuvem of Oort. Crystals require high temperatures to form, above 900 K, which does not occur in external areas. The observations of Webb indicate that the process takes place in the inner part of the disk, equivalent to the distance between Sol and Terra in mature systems.
Protostar EC 53 goes through predictable cycles of accretion bursts every 18 months, lasting about 100 days. During these periods, the star rapidly consumes gas and dust, generating jets and winds that eject the newly formed silicates. Essa dynamics allow crystals to reach distant regions, where they can incorporate themselves into icy bodies such as comets.
Detailed observations with the MIRI instrument
Mid-Infrared Instrument (MIRI) instrument on James Webb captured detailed two-phase spectra of the protostar EC 53. Esses data revealed the specific presence of minerals such as forsterite and enstatite in the dust near the star. The analysis mapped changes during the quiet period and the active burst.
The spectra indicated that crystalline silicates form exclusively in the scorching inner zone of the disc. Strong Ventos, originating in this region, act as an efficient transport mechanism for tiny particles.
Activity cycle of the protostar EC 53
The EC 53 protostar features regular outbursts, studied for decades by international teams. Cada cycle lasts approximately 100 days and occurs at 18-month intervals. Nessa phase, accretion accelerates and ejects material in high-speed polar jets.
The slower outflows, coming from the inner area of the disk, carry the newly formed crystalline silicates. Essa ejection directs the crystals to the cold ends, where conditions allow future comet formation.
Types of silicates identified
Observations of Webb confirmed common minerals in Terra among crystalline silicates. The main ones include:
- Forsterite, a magnesium-rich silicate often found in terrestrial rocks.
- Enstatite, another silicate mineral present in meteorites and the planetary crust.
- Particles smaller than grains of sand, formed at high temperatures.
These compounds represent basic ingredients for rocky planets. Sua detection in EC 53 reinforces models of planetary formation in young disks.
Disk transport mechanism
Illustrations based on the data show half of the protoplanetary disk of EC 53. Periodic Outbursts generate crystalline silicates in the hot central region. Ventos and jets direct particles upward and outward.
The crystals travel like a cosmic highway to the icy edges. Lá, can be incorporated into rocky and icy bodies in formation. The process occurs on a scale comparable to Earth’s orbit at Sistema Solar.
Polar jets appear narrow and fast in MIRI observations. Wider and slower Outflows depart from the star’s feeding zone.
Context in Nebulosa of Serpens
Nebulosa of Serpens is home to thousands of actively forming protostars. EC 53 integrates this environment rich in gas and dust. The region is 1,300 light-years from Terra and serves as a natural laboratory for studies of star birth.
The EC 53 disk remains encased in opaque material for another approximately 100,000 years. Colisões among dust grains and boulders build larger bodies over millions of years.
Instruments used in observations
The Near-Infrared Camera (NIRCam) captured initial images of EC 53 in 2024. Essas views highlighted scattered winds and reflected light from the disk. An angled white half-moon represents a set of outflows in the image.
MIRI provided mid-infrared spectra to identify chemical compositions. The combination of instruments made it possible to map the exact positions of the silicates before and during bursts.
International team and publishing
Researchers led by Jeong-Eun Lee, of Universidade Nacional of Seul, analyzed the data. Coautores include Doug Johnstone, from Conselho Nacional from Pesquisa from Canadá, and Joel Green, from Space Telescope Science Institute. The study appeared in the journal Nature.
The team highlighted Webb’s ability to reveal specific minerals in space. Esses findings connect processes in young systems to the composition of current Sistema Solar.
Future evolution of the system
EC 53’s disk will evolve over millions of years with constant collisions. Tiny Grãos aggregate into rocks and terrestrial planets or gas giants. The remaining material gradually clears the view of the center.
A star similar to Sol will remain at the core of a mature planetary system. Silicatos crystals are distributed throughout the environment, including in peripheral comets.