Эрдэмтэд залуу оддыг хүрээлсэн хийн дискүүд хэрхэн өөрчлөгдөж, гариг бүрэлдэхэд шаардлагатай түүхий эдээ алдаж буйг судалжээ.
Аризонагийн их сургуулийн судлаач Наман Бажаж болон SETI хүрээлэнгийн Ума Горти нараар ахлуулсан олон улсын баг Жэймс Вэбб сансрын дурангийн MIRI багажийг ашиглан 72 залуу, Нар шиг оддыг судалжээ. Судалгаагаар гариг үүсэх явцад эдгээр оддыг тойрсон хий болон тоосонцрын дискнүүд хэрхэн хувьсан өөрчлөгдөж, хийн алдагдлын улмаас гариг үүсэх боломж хэрхэн хязгаарлагдаж байгааг тогтоосон байна. Энэхүү үр дүн нь The Astronomical Journal сэтгүүлд хэвлэгджээ.
Судалгаанд хамрагдсан хамгийн залуу системүүдэд соронзон хүчээр үүсгэгдсэн салхи болон тийрэлтэт урсгалууд давамгайлж байгаа нь ажиглагдсан байна. Эрдэмтэд молекул устөрөгч болон ионжсон неоны дохиог хянах замаар эдгээр урсгал нь дискний материалыг одны орчмоос зайлуулах үүрэгтэйг тогтоожээ. Нийт 72 дискний 66-д нь ийм төрлийн урсгал илэрсэн бөгөөд 46 системд конус хэлбэрийн молекул устөрөгчийн салхи, 40 системд хурдтай неон тийрэлтэт урсгал бүртгэгдсэн байна.
Системүүд нас ахих тусам соронзон урсгалууд суларч, оронд нь одны өндөр энергитэй цацрагийн нөлөөгөөр хийг ууршуулах буюу фото-ууршилтын процесс давамгайлж эхэлдэг болохыг судалгаа харуулжээ. Энэхүү үйл явц нь Бархасбадь, Санчир зэрэг аварга гаригууд агаар мандлаа бүрдүүлэхэд шаардлагатай хийг дискнээс татан авах хугацааг тодорхойлдог байна.
Наман Бажаж гариг үүсэх үйл явцыг цаг хугацаатай уралдах уралдаан хэмээн тодорхойлсон бөгөөд дискэн дэх хий салхи болон цацрагийн нөлөөгөөр бүрэн алга болохоос өмнө аварга гаригууд бүрэлдэж амжих ёстой гэдгийг онцолжээ. Судлаачид цаашид хийн алдагдлын хэмжээг нарийвчлан тодорхойлох замаар гариг үүсэх боломжит хугацааны хязгаарыг бүрэн тодруулахаар ажиллаж байна.
Дэлгэрэнгүйг эх сурвалжаас харах
↓Эх сурвалжийг нээх ↓
NASA’s James Webb Space Telescope (JWST) has revealed that young planetary systems lose their gas through different processes as they age. The discovery shows that the formation of giant planets depends on a changing battle between planet growth and the winds that remove their building material.
A team of astronomers studied 72 young, Sun-like stars to track how protoplanetary disks evolve during the first stages of planetary formation. Led by Naman Bajaj of the University of Arizona and co-authored by Uma Gorti of the SETI Institute, the research provides a detailed look at how gas disappears from these planet-forming environments.
Gas inside these disks provides the raw material needed to create planets, including the massive atmospheres of worlds such as Jupiter and Saturn. The young solar system also passed through this phase, when the early Sun was surrounded by a dense disk containing far more gas than dust before most of that material was lost.
Published in The Astronomical Journal, the study uses JWST observations from the telescope’s Mid-Infrared Instrument (MIRI) to compare planetary systems at different ages. The researchers found that the mechanisms removing gas from these disks change as the systems mature.
Magnetic Winds Shape Young Planetary Disks
The youngest systems in the survey showed strong evidence of magnetically driven winds and jets. These outflows are powered by magnetic fields connected to the disk and can transport gas and angular momentum away from the developing planetary system.
To study these processes, the team examined two key signals: molecular hydrogen and ionized neon. Molecular hydrogen traces broad winds carrying large amounts of disk material, while ionized neon reveals faster-moving jets and atomic outflows.
The observations confirm predictions made before JWST could directly detect some of these molecular winds. Earlier research led by Ilaria Pascucci proposed that young disks could produce molecular outflows capable of affecting how high-energy radiation interacts with the surrounding material.
The survey detected extended molecular hydrogen and ionized neon emissions in 66 of the 72 disks. Conical molecular hydrogen winds were identified in 46 systems, while 40 systems displayed fast-moving neon jets. The results show that several wind mechanisms can operate during the earliest stages of planetary evolution.
Radiation Winds Grow Stronger With Age
The study shows that the balance between different gas-loss processes changes as young systems develop. When less material continues to fall onto the central star, the powerful jets and molecular winds seen in younger disks begin to weaken. At later stages, photoevaporation becomes increasingly important. This process occurs when high-energy radiation from the young star penetrates deeper into the disk, heats the gas, and allows it to escape.
The research connects decades of theoretical work on ultraviolet and X-ray driven winds with direct observations across a large sample of young stars. Uma Gorti has spent years studying how radiation influences the disappearance of protoplanetary disks, and the new JWST results provide measurements that show this transition taking place.
The findings indicate that disk dispersal is controlled by several processes rather than a single mechanism. Young systems begin with strong magnetic activity, then gradually shift toward gas loss driven by radiation as their disks evolve.
Giant Planets Must Form Before Gas Runs Out
The changing nature of disk winds creates a limited period for the formation of gas giants. Planets like Jupiter need access to large quantities of gas while the surrounding disk still contains enough material to build their atmospheres.
“Planet formation is therefore a race against time,” said Naman Bajaj. “Gas giants like Jupiter must assemble their massive atmospheres while the disk is still substantial enough to supply them, before winds and jets carry that raw material away into space.”
The new study expands previous JWST observations of the young star T Cha, where researchers directly observed gas being removed from a planet-forming disk. By analyzing dozens of systems, astronomers can now examine how jets, molecular winds, and atomic winds change throughout early planetary evolution.
The researchers are continuing to study how much gas these winds remove and which parts of the disk provide the escaping material. These measurements will help clarify how long young planetary systems can continue forming different types of planets before their gas reservoirs disappear.
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