Recent observations have uncovered a spiral pattern in the material disk surrounding a young, high-mass protostar, suggesting the presence of gravitational instability within the disk. This finding carries significant implications for how high-mass stars form. During the process of star formation
Map of material distribution in the disk around protostar G358-MM1. The white “+” marks the location of the protostar. The contour lines indicate signal strength. The colors represent the line-of-sight velocities. Movement away from the viewer is shown in red/orange and movement towards the viewer is shown in blue/green, indicating that the disk is rotating. Overlaid gray lines indicate the spiral arms identified through data analysis. Credit: R. A.
During the process of star formation, a protostellar disk serves as a means of delivering material to the nascent “protostar” at its core. In the case of high-mass protostars that have already surpassed 8 times the mass of the Sun and continue to grow, it is hypothesized that instead of a steady stream, clusters of material periodically descend from the disk onto the protostar, triggering brief but intense growth spurts.
The observational results show clear rotation around the central protostar and a spiral pattern with four arms. Spiral arms in rotating protostellar disks are a sign of instability, a characteristic which was long theorized to be associated with massive star formation, but had yet to be proven observationally.
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