This image gallery of stellar winds around cool ageing stars shows a variety of morphologies, including disks, cones, and spirals. The blue color represents material that is coming towards you; red is material that is moving away from you.
Credit: L. Decin, ESO/ALMA

 
Dying stars swell and cool to eventually become red giants. They produce stellar winds, flows of particles that the star expels, which causes them to lose mass. Because detailed observations were lacking, astronomers have always assumed that these winds were spherical, like the stars they surround. As the star evolves further, it heats up again, and the stellar radiation causes the expanding ejected layers of stellar material to glow, forming a planetary nebula.

For centuries, astronomers were in the dark about the extraordinary variety of colorful shapes observed in planetary nebulas. The nebulae all seem to have a certain symmetry but are rarely round. “The Sun – which will ultimately become a red giant – is as round as a billiard ball, so we wondered: how can such a star produce all these different shapes?” says corresponding author Leen Decin (KU Leuven).

Her team observed stellar winds around cool red giant stars with the ALMA observatory in Chile, the world’s largest radio telescope. For the first time, they gathered an extensive, detailed collection of observations. Each of them made using the same method, crucial to compare the data, and exclude biases directly.

What the astronomers saw surprised them. “We noticed these winds are anything but symmetrical or round,” Professor Decin says. “Some of them are quite similar in shape to planetary nebulae.”

The researchers could even identify different categories of shapes. “Some stellar winds were disk-shaped, others contained spirals, and we identified cones in a third group.” This is a clear indication that the shapes weren’t created randomly. The team realized that other low-mass stars or even heavy planets in the dying star’s vicinity were causing the different patterns. These companions are too small and dim to detect directly. “Just like how a spoon that you stir in a cup of coffee with some milk can create a spiral pattern, the companion sucks material towards it as it revolves around the star and shapes the stellar wind,” Decin explains.

The team put this theory into models, and indeed: the shape of the stellar winds can be explained by the companions surrounding them. The rate at which the cool evolved star is losing its mass due to the stellar wind is an important parameter.

Up until now, calculations about the evolution of stars were based on the assumption that aging Sun-like stars have spherical stellar winds. “Our findings change a lot. Since the complexity of stellar winds was not accounted for in the past, any previous mass-loss rate estimate of old stars could be wrong by up to a factor of 10.” The team is now doing further research to see how this might impact calculations of other crucial characteristics of stellar and galactic evolution.

The study also helps envision what the Sun might look like when it dies in 7000 million years. “Jupiter or even Saturn – because they have such a big mass – are going to influence whether the Sun spends its last millennia at the heart of a spiral, a butterfly, or any of the other entrancing shapes we see in planetary nebulae today,” Decin notes. “Our calculations now indicate that a weak spiral will form in the stellar wind of the old dying Sun.”

“We were very excited when we explored the first images,” says co-author Miguel Montargès (KU Leuven). “Each star, which was only a number before, became an individual by itself. Now, to us, they have their own identity. This is the magic of having high-precision observations: stars are no longer just points anymore.”

The study is part of the ATOMIUM project, which aims to learn more about the physics and chemistry of old stars. “Cool aging stars are considered boring, old and simple, but we now prove that they are not: they tell the story of what comes after. It took us some time to realize that stellar winds can have the shape of rose petals (see, for example, the stellar wind of R Aquilae). But, as Antoine de Saint-Exupéry said in his book Le Petit Prince: ‘C’est le temps que tu as perdu pour ta rose, qui fait ta rose si importante’ – ‘It’s the time you spent on your rose that makes your rose so important,’” Decin concludes.

This article is based on the news release issued by the Joint ALMA Observatory.

 
Paper Information

These observation results were published as L. Decin et al. “(Sub)stellar companions shape the winds of evolved stars” in the journal Science on 18 September 2020.

The Atacama Large Millimeter/submillimeter Array (ALMA), an international astronomy facility, is a partnership of the European Organisation for Astronomical Research in the Southern Hemisphere (ESO), the U.S. National Science Foundation (NSF) and the National Institutes of Natural Sciences (NINS) of Japan in cooperation with the Republic of Chile. ALMA is funded by ESO on behalf of its Member States, by NSF in cooperation with the National Research Council of Canada (NRC) and the Ministry of Science and Technology (MOST) and by NINS in cooperation with the Academia Sinica (AS) in Taiwan and the Korea Astronomy and Space Science Institute (KASI).

ALMA construction and operations are led by ESO on behalf of its Member States; by the National Radio Astronomy Observatory (NRAO), managed by Associated Universities, Inc. (AUI), on behalf of North America; and by the National Astronomical Observatory of Japan (NAOJ) on behalf of East Asia. The Joint ALMA Observatory (JAO) provides the unified leadership and management of the construction, commissioning and operation of ALMA.