Astronomers revealed details about the structure of the large protostellar disk known as G358-MM1. This finding was reported by TASS, citing the press service of the Ural Federal University, whose researchers participate in an international collaboration of scientists.
A protostellar accretion disk is a cloud of interstellar gas that gradually contracts under gravity. As the density and temperature in the cloud increase to a critical point, nuclear reactions ignite. In the early stages of evolution, such disks may display complex features beyond a simple spherical shape.
Until recently, the precise architecture of disks around massive protostars remained unknown. The new observations provide evidence that the disk around a large protostar possesses a structured form with four spiral arms. Material appears to flow along these spirals toward the inner regions of the disk, eventually feeding the central protostar. The study employed a novel technique called excitation-wave mapping, which uses bursts of stellar radiation to illuminate the disk material and make methanol molecules glow, revealing the dynamics of the gas. The researchers noted that implementing this method posed significant challenges. (Source: TASS)
Understanding the architecture of protostars is essential for grasping the evolution of the universe and the formation of planetary systems within it. The insights gained from these observations add a crucial piece to the long-standing puzzle of how stars accumulate mass and how surrounding disks organize the flow of material toward the forming star.
These findings also contribute to broader questions about the origin of cosmic structures. By mapping the structure and motion within protostellar disks, scientists can refine theories about early stellar development and the conditions that lead to planet formation in diverse environments. The work underscores the importance of high-resolution observational techniques and international collaboration in advancing our knowledge of stellar birth and the history of our own solar neighborhood.