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Winds blowing off a dying star

Japanese scientists use ALMA to explain aluminum oxide enrichment around AGB stars

Kyoto University

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IMAGE: High spatial-resolution image of AlO and SiO molecules around AGB star W Hydrae, observed using ALMA, with AlO molecule emissions in red and those from SiO molecules and the star... view more 

Credit: ALMA [ESO/NAOJ/NRAO], Takigawa et al, Kyoto University

Japan -- Stars like our Sun eject large amounts of gas and dust into space, containing various elements and compounds. Asymptotic giant branch -- AGB -- phase stars, near their end of life, are particularly significant sources of such substances in our galaxy.

Formation of dust around AGB stars has been considered to play an important role in triggering acceleration of stellar wind, but the detailed mechanism of this acceleration has not been well explained.

And there is yet another conundrum. In space, silicon is ten times more abundant than aluminum. However, many oxygen-rich AGB stars are rich in aluminum oxide dust -- the major carrier of aluminum -- but poor in silicate dust -- the carrier of silicon, which has puzzled researchers: why is aluminum oxide dust so abundant around oxygen-rich AGB stars?

In a paper published in Science Advances, a research team led by Aki Takigawa of Kyoto University have utilized the Atacama Large Millimeter/submillimeter Array -- ALMA, as the high spatial-resolution radio interferometer in Chile is known -- to obtain detailed images of gas molecules forming dust surrounding an AGB star.

"Previously, there was a limit to how well we could observe dust forming regions close to stars," explains Takigawa. "Now, thanks to the high spatial resolution of ALMA, we can obtain images of gases in these regions in finer detail. So we pointed ALMA toward an aluminum oxide-rich AGB star, W Hydrae."

Gas molecules aluminum monoxide and silicon monoxide -- AlO and SiO -- eventually form aluminum oxide and silicate dust. The team observed that AlO was distributed within three stellar radii of W Hydrae, which was surprisingly similar to the previously-observed dust distribution.

Meanwhile, SiO was detected beyond five stellar radii, and moreover 70% remained gaseous, without forming into dust.

"These results indicate that as aluminum oxide grows and accumulates near a star, the addition of a small amount of silicate dust may trigger wind acceleration," elaborates Takigawa. "This decreases gas density, suppressing further silicate dust formation."

"This may explain the presence of aluminum-oxide-rich but silicate-poor AGB stars."

These new results shed light not only on the dynamics of gas and dust surrounding stars, but also on the importance of studying both together. The team plans to continue using ALMA to elucidate gas and dust dynamics in the universe.

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The paper "Dust formation and wind acceleration around the aluminum oxide-rich AGB star W Hydrae" appeared 1 November 2017 in Science Advances, with doi: 10.1126/sciadv.aao2149

Kyoto University is one of Japan and Asia's premier research institutions, founded in 1897 and responsible for producing numerous Nobel laureates and winners of other prestigious international prizes. A broad curriculum across the arts and sciences at both undergraduate and graduate levels is complemented by numerous research centers, as well as facilities and offices around Japan and the world. For more information please see: http://www.kyoto-u.ac.jp/en

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