Astronomers have used a large millimeter / submillimeter array (Alma) to answer the main questions about stars. The question is, do a much bigger star than our solar form in the same way as smaller stars. Astronomers have observed the stars that are still formed similar to the sun when they get material from the cloud of dust and gas around it relatively quickly. The mass of ingredients entered into a disk that orbits young stars that feed stars at fast speeds to digest.
The material remaining in the orbit disk finally forms a fixed planet after the star growth process is complete. This type of disk is generally seen around the stars that are low but have not been found around a much larger star in the initial formation stage. Astronomers have tried to answer questions whether the process for larger stars is similar to the process used by a smaller star or something completely different.
Astronomer Ciriaco Goddi from Radboud University Nijmegen in the Netherlands said his team used Alma’s observations to study three young stars in high mass in the star-known region as W51. For their research, the team uses Alma with its intention spread separately with their widest point, giving the power to complete the image ten times sharper than the previous object study.
Astronomers looked for evidence that a stable big disc was seen orbiting smaller young stars also orbiting a bigger star. With a larger Alma power, the researchers hope to see the disk around larger stars but instead find the meal zone that looks like a chaotic mess. The researchers concluded that large stars at the early stages of drawing material for various directions at an unstable level, which is very different from smaller stars.
Some material channels that enter developing stars may prevent large and steady disc formation seen around smaller stars. Scientists are not so surprised in this case because what is called the “disordered involved” model is proposed based on computer simulation. This marks the first observational evidence to support the model.
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