Final kiss of two stars heading for catastrophe

This artist’s impression shows VFTS 352 — the hottest and most massive double star system to date where the two components are in contact and sharing material. The two stars in this extreme system lie about 160,000 light-years from Earth in the Large Magellanic Cloud. This intriguing system could be heading for a dramatic end, either with the formation of a single giant star or as a future binary black hole.

ESO/L. Calçada

Using ESO’s Very Large Telescope (VLT), an international team of astronomers has found the hottest and most massive double star with components so close that they touch each other. The two stars in the extreme system VFTS 352 could be heading for a dramatic end, during which the two stars either coalesce to create a single giant star or form a binary black hole.

The double star system VFTS 352 is located about 160,000 light-years away in the Tarantula Nebula. This remarkable region is the most active nursery of new stars in the nearby universe, and new observations from ESO’s VLT have revealed that this pair of young stars is among the most extreme and strangest yet found.

VFTS 352 is composed of two hot, bright, and massive stars that orbit each other in little more than a day. The centers of the stars are separated by just 7.5 million miles (12 million kilometers). In fact, the stars are so close that their surfaces overlap and a bridge has formed between them. VFTS 352 is not only the most massive known in this tiny class of “over-contact binaries,” but also has a combined mass of about 57 times that of the Sun — it also contains the hottest components with surface temperatures above 72,000° F (40,000° C).

Extreme stars like the two components of VFTS 352 play a key role in the evolution of galaxies and are thought to be the main producers of elements such as oxygen. Such double stars are also linked to exotic behavior such as that shown by “vampire stars,” where a smaller companion star sucks matter from the surface of its larger neighbor.

In the case of VFTS 352, however, both stars in the system are of almost identical size. Material is, therefore, not sucked from one to another, but instead may be shared. The component stars of VFTS 352 are estimated to be sharing about 30 percent of their material.

Such a system is rare because this phase in the life of the stars is short, making it difficult to catch them in the act. Because the stars are so close together, astronomers think that strong tidal forces lead to enhanced mixing of the material in the stellar interiors.

“The VFTS 352 is the best case yet found for a hot and massive double star that may show this kind of internal mixing,” said Leonardo A. Almeida of the University of São Paulo, Brazil. “As such, it’s a fascinating and important discovery.”

Astronomers predict that VFTS 352 will face a cataclysmic fate in one of two ways. The first potential outcome is the merging of the two stars, which would likely produce a rapidly rotating and possibly magnetic gigantic single star. “If it keeps spinning rapidly, it might end its life in one of the most energetic explosions in the universe, known as a long-duration gamma-ray burst,” said Hugues Sana from the University of Leuven in Belgium.

Selma de Mink of the University of Amsterdam explained the second possibility: “If the stars are mixed well enough, they both remain compact and the VFTS 352 system may avoid merging. This would lead the objects down a new evolutionary path that is completely different from classic stellar evolution predictions. In the case of VFTS 352, the components would likely end their lives in supernova explosions, forming a close binary system of black holes. Such a remarkable object would be an intense source of gravitational waves.”

Proving the existence of this second evolutionary path would be an observational breakthrough in the field of stellar astrophysics. But regardless of how VFTS 352 meets its demise, this system has already provided astronomers with valuable new insights into the poorly understood evolutionary processes of massive over-contact binary star systems.

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