December 12, 2021
In the not-so-distant past, the discovery of a supernova – an exploding star – was considered a rare occasion. For example, when Professor Avishay Gal-Yam of the Weizmann Institute’s Particle Physics and Astrophysics Department and Dean of Weizmann’s Physics Faculty, was a doctoral student he located seven over the course of four years.
Now things have changed. Today, published in Nature, Gal-Yam and colleagues had their recent discovery of a rare-type supernova never observed before revealed.
Advanced measuring instruments and analysis methods today make it possible to detect fifty general supernova explosions on a daily basis. On one hand, this improved means used by astrophysicists to spot supernovae may have made these celestial events less of an attraction over the years; on the other, the increased observations have raised the probability that researchers would spot these rarer types of explosions like the one just discovered, which before were only theoretical.
So how does it work? The core of every star is fuelled by nuclear fusion, wherein the nuclei of lighter elements fuse together to form heavier elements. The fusion of four hydrogen nuclei results in the formation of a helium atom, while several helium nuclei combined result in the formation of carbon, oxygen, and so on.
The last element that will naturally form through nuclear fusion is iron, which is the most stable atomic nucleus. In normal circumstances, the energy produced at the star’s core maintains extremely high temperatures that cause its gaseous matter to expand, thus preserving the fine balance with the force of gravity, drawing the star’s mass toward its centre.
Once the star runs out of elements to fuse and stops producing energy, this balance is disrupted, leading either to a gaping black hole that tears open at the heart of the star, causing it to collapse in on itself, or to the star’s explosion, which releases the heavy elements, fused during its evolution, into the universe.
The entire process is naturally very lengthy. The life spans of massive stars – the kind that Gal-Yam studies – are considered relatively short, a few million years at most. The Sun, in comparison, has a life expectancy of about 10 billion years.
The subsequent processes of nuclear fusion at the core of massive stars lead to their stratification, in which the heavy elements are concentrated at the core, and gradually lighter elements compose the outer layers.
Wolf-Rayet stars are particularly massive stars that are missing one or more of the external layers that are made up of lighter elements. In this way, instead of hydrogen – the lightest element – the star’s surface is characterised by the presence of helium, or even carbon and heavier elements.
One possible explanation for this phenomenon is that strong winds blowing due to high pressure at the star’s envelope, disperse its outermost layer, causing the star to lose one layer after the other over several hundred thousand years. When these stars are observed without the presence of the lighter elements in their envelope, it is akin to a still photograph capturing a moment in time during a long-winded process. Nonetheless, despite their relatively short life spans and their state of progressive disintegration, the supernova explosion of a Wolf-Rayet star has yet to have been definitely observed.
Analysis of the ever-growing number of supernova discoveries has led to the hypothesis that Wolf-Rayet stars simply don’t explode – they just quietly collapse into black holes – otherwise, we would have been able to observe one by now.
This hypothesis, however, has just been shattered owing to the discovery, made by the Weizmann group and their international team of collaborators, of a supernova originating from this type of star.
Spectroscopic analysis of the light emitted from the explosion – the electromagnetic wavelengths of light emitted from the blast – led to the discovery of spectral signatures that are associated with specific elements. In this way, the researchers were able to show that the explosion contained carbon, oxygen and neon atoms, the latter an element that has not yet been observed in this manner in any supernova to date.
Moreover, the researchers identified that the matter spouting cosmic radiation did not in itself participate in the blast but rather originated from the space surrounding the volatile star. This, in turn, strengthened their hypothesis in favor of strong winds that took part in stripping the star of its outer envelope.
Since this observation is the first of its kind, Gal-Yam states that it may be too early to unequivocally determine the fate of all such stars.
“We can’t say at this stage whether all Wolf-Rayet stars end their lives with a bang or not. It might be that some of them do collapse quietly into a black hole,” he said.
“We estimate that the mass that dispersed during the explosion is probably equal to that of the Sun or a slightly smaller star; the star that exploded was significantly heavier – having a mass at least ten times greater than that of the Sun. So where did the majority of mass end up?”
Gal-Yam suggests a midway scenario, in which both possible fates are fulfilled at the same time: once nuclear fusion is exhausted at the star’s core, an explosion takes place that blasts some of the mass into space, while the remaining mass collapses in on itself, forming a black hole.
“One thing’s certain, this is not the ‘silent’ collapse often referred to in the past. It’s worth mentioning that since this discovery was first made, another similar explosion of a Wolf-Rayet star has been observed, implying that this phenomenon is indeed not a single occurrence,” said Gal-Yam.
“It is possible that the better our detection and measurement instruments become, the more this type of explosion – today considered rare and exotic – will become a common sight.”
Supernovae may seem like colossal events happening far, far away that they have no direct impact on our lives. But, truth be told, they are at the heart of life itself.
These cosmic explosions launch the elements that were forged at the star’s core to the far reaches of the galaxy, where they serve as the bedrock for the birth of new stars. Planet Earth and all its various and diverse life-forms (including us Homo sapiens) are the result of such an occurrence.
“We study the origins of all matter, including that found on Earth, and search for explanations of many of the physical phenomena we tend to take for granted. This is what I am personally interested in – where did all of this come from – and I want to be able to answer this question as best and as accurately as I can,” concluded Gal-Yam.
Here we see the spectacular cosmic pairing of the star Hen 2-427 — more commonly known as WR 124 — and the nebula M1-67 which surrounds it. Both objects, captured here by the NASA/ESA Hubble Space Telescope are found in the constellation of Sagittarius and lie 15 000 light-years away. The star Hen 2-427 shines brightly at the very centre of this explosive image and around the hot clumps of gas are ejected into space at over 150 000 kilometres per hour. Hen 2-427 is a Wolf–Rayet star, named after the astronomers Charles Wolf and Georges Rayet. Wolf–Rayet are super-hot stars characterised by a fierce ejection of mass. The nebula M1-67 is estimated to be no more than 10 000 years old — just a baby in astronomical terms — but what a beautiful and magnificent sight it makes. A version of this image was released in 1998, but has now been re-reduced with the latest software.
The Israeli research team from the Particle Physics and Astrophysics Department at the Weizmann Institute of Science