Oglądanie gwałtownej śmierci bardzo gigantycznej gwiazdy jest rzadkością

Red Hypergiant Star VY Canis Majoris

Artystyczna wizja czerwonego olbrzyma VY Canisa Majorisa. VY Canis Majoris znajduje się około 3009 lat świetlnych od Ziemi i jest prawdopodobnie najmasywniejszą gwiazdą Drogi Mlecznej. Źródło: NASA/ESA/Hubble/R. Humphreys, University of Minnesota/J. Olmsted, STScI/hublesite.org

Śledząc emisje molekularne w wypływach wokół czerwonego olbrzyma VY Canis Majoris, astronomowie uzyskali pierwszą szczegółową mapę atmosfery gwiazdy, która rzuca światło na mechanizmy zaangażowane w końcowe stadia ekstremalnego olbrzyma.

Zespół astronomów kierowany przez Uniwersytet w Arizonie stworzył szczegółowy obraz 3D umierającej gwiazdy olbrzyma. Zespół kierowany przez badaczy z UArizona, Ambesha Singha i Lucy Ziurys, śledził rozkład, kierunki i prędkości różnych cząstek otaczających czerwonego olbrzyma, znanego jako VY Canis Majoris.

Ich odkrycia, które zaprezentowali 13 czerwca 2022 r. na 240. spotkaniu Amerykańskiego Towarzystwa Astronomicznego w Pasadenie w Kalifornii, oferują wgląd na bezprecedensową skalę na temat procesów towarzyszących śmierci gigantycznych gwiazd. Ze współpracownikami współpracowali Robert Humphreys z University of Minnesota i Anita Richards z University of Manchester w Wielkiej Brytanii.

Ekstremalne olbrzymy zwane hiperolbrzymami są bardzo rzadkie i tylko nieliczne są o nich znane[{” attribute=””>Milky Way. Examples include Betelgeuse, the second brightest star in the constellation Orion, and NML Cygni, also known as V1489 Cygni, in the constellation Cygnus. Unlike stars with lower masses – which are more likely to puff up once they enter the red giant phase but generally retain a spherical shape – hypergiants tend to experience substantial, sporadic mass loss events that form complex, highly irregular structures composed of arcs, clumps, and knots.

Located about 3,009 light-years from Earth, VY Canis Majoris – or VY CMa, for short – is a pulsating variable star in the slightly southern constellation of Canis Major. Spanning anywhere from 10,000 to 15,000 astronomical units (with 1 AU being the average distance between Earth and the sun) VY CMa is possibly the most massive star in the Milky Way, according to Ziurys.

“Think of it as Betelgeuse on steroids,” said Ziurys, a Regents Professor with joint appointments in UArizona Department of Chemistry and Biochemistry and Steward Observatory, both part of the College of Science. “It is much larger, much more massive and undergoes violent mass eruptions every 200 years or so.”

The team chose to study VY CMa because it is one of the best examples of these types of stars.

“We are particularly interested in what hypergiant stars do at end of their lives,” said Singh, a fourth-year doctoral student in Ziurys’ lab. “People used to think these massive stars simply evolve into supernovae explosions, but we are no longer sure about that.”

“If that were the case, we should see many more supernovae explosions across the sky,” Ziurys added. “We now think they might quietly collapse into black holes, but we don’t know which ones end their lives like that, or why that happens and how.”

Previous imaging of VY CMa with NASA’s Hubble Space Telescope and spectroscopy showed the presence of distinct arcs and other clumps and knots, many extending thousands of AU from the central star. To uncover more details of the processes by which hypergiant stars end their lives, the team set out to trace certain molecules around the hypergiant and map them to preexisting images of the dust, taken by the Hubble Space Telescope.

“Nobody has been able to make a complete image of this star,” Ziurys said, explaining that her team set out to understand the mechanisms by which the star sheds mass, which appear to be different from those of smaller stars entering their red giant phase at the end of their lives.

“You don’t see this nice, symmetrical mass loss, but rather convection cells that blow through the star’s photosphere like giant bullets and eject mass in different directions,” Ziurys said. “These are analogous to the coronal arcs seen in the sun, but a billion times larger.”

The team used the Atacama Large Millimeter Array, or ALMA, in Chile to trace a variety of molecules in material ejected from the stellar surface. While some observations are still in progress, preliminary maps of sulfur oxide, sulfur dioxide, silicon oxide, phosphorous oxide and sodium chloride were obtained. From these data, the group constructed an image of the global molecular outflow structure of VY CMa on scales that encompassed all ejected material from the star.

“The molecules trace the arcs in the envelope, which tells us molecules and dust are well-mixed,” Singh said. “The nice thing about emissions of molecules at radio wavelengths is that they provide us with velocity information, as opposed to the dust emission, which is static.”

By moving ALMA’s 48 radio dishes into different configurations, the researchers were able to obtain information about the directions and velocities of the molecules and map them across the different regions of the hypergiant’s envelope in considerable detail, even correlating them to different mass ejection events over time.

Processing the data required some heavy lifting in terms of computing power, Singh said.

“So far, we have processed almost a terabyte from ALMA, and we still receive data that we have to go through to get the best resolution possible,” he said. “Just calibrating and cleaning the data requires up to 20,000 iterations, which takes a day or two for each molecule.”

“With these observations, we can now put these on maps on the sky,” Ziurys said. “Until now, only small portions of this enormous structure had been studied, but you can’t understand the mass loss and how these big stars die unless you look at the entire region. That’s why we wanted to create a complete image.”

With funding from the National Science Foundation, the team plans to publish its findings in a series of papers.

Meeting: 240th meeting of the American Astronomical Society

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About the Author: Ellen Doyle

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