2023.2.28 preparation

Spiral arm high-mass protostellar accretion disk revealed by radio telescopes

科学研究部の Dr. Burns Rossらの研究成果が発表されました。
Nature astronomyに2023年2月27日付で掲載されています。

High-mass stars are 8 or more times more massive than the Sun. They act like atomic factories to generate many of the necessary building blocks for life in the universe and they alter the appearance and evolution of galaxies. The most massive stars become enigmatic black holes when they die. Despite their importance in the Universe, the process by which high-mass stars are born is unclear. 

Thanks to the efforts of many astronomers and engineers we now have telescopes capable of seeing the birth sites of high-mass stars, also known as ‘high-mass protostars’, in more and more detail. We now know that they form at the hearts of rotating disks of gas and dust which are ~1000 AU radius (that is, ~1000 times the distance at which the Earth orbits the Sun). 

However, the exact process by which material from the disk feeds the protostar has been a mystery for many decades. Many theories have proposed ideas about how material from the disk reaches the protostar. One such theory is that of episodic, disk-fed accretion, which is characterized by short bursts of accretion, separated by low-activity states which can last months to years. In a paper published in Nature Astronomy in 2020, a group led by NAOJ astronomer Ross Burns described a ‘heat-wave’ that was seen traversing the accretion disk in high-mass protostar, G358-MM1, shortly following its accretion burst. The finding was consistent with episodic disk-fed accretion.

Figure 1: Artist’s impression of the G358-MM1 spiral arm accretion disk. Credit: Charlie Willmott and Ross Burns

Burns and his team, have now made further progress in the understanding of the birth of high-mass stars. Using VLBI arrays from around the world in an international collaboration, the team were able to discover spiral arms in the rotating disk of high-mass protostar, G358-MM1. Spiral arms are thought to occur due to the disk becoming unstable when it grows too massive. G358-MM1 has four spiral arms which wrap beautifully around the protostar. The spiral arms help to feed disk material down to the inner radius of the system where it can reach the protostar and feed it. Since the protostar, G358-MM1, already has been observed to undergo growth bursts the discovery of a spiral instability helps to associate the role of disk instability into the process of high-mass star formation. In fact, this association has been proposed in theoretical hypotheses since many years ago but was not confirmed by observations until now.

Burns’ team used a new technique called ‘heat-wave mapping’ which used the growth burst’s own flash of radiation to map the surface of the disk using methanol masers.
The team will continue to search for growth bursts in high-mass protostars, using a global cooperative of traditional radio telescopes, called the Maser Monitoring Organisation (M2O). So far, only 3 high-mass protostellar bursts have been seen, Burns’ team hopes to find many more to explore more growth bursts in other high-mass protostars.

Figure 2: VLBI Image of the methanol masers in G358-MM1 revealed using heat-wave mapping. Contours indicate brightness which traces the spiral arms which are highlighted as white lines. Colours indicate the motion of the gas where red shows gas moving away from us and blue shows gas moving toward us. The colours reveal disk rotation. The protostar resides at the center of the disk.

If more spiral systems and growth bursts are discovered in other high-mass protostars, either using heat-wave mapping or other observational techniques, then astronomers will be able to provide a better understanding of the births of high-mass stars, which are the energetic progenitors of life in the Universe.

Nature astronomy: https://www.nature.com/articles/s41550-023-01899-w
国立天文台(日本語版): https://www.nao.ac.jp/news/science/2023/20230228-dos.html
国立天文台(英語版): https://www.nao.ac.jp/en/news/science/2023/20230228-dos.html