This is what we’ll see when Betelgeuse goes supernova

The stars in the night sky, as we typically perceive them, are normally static and unchanging to our eyes. Sure, there are variable stars that brighten and fainten, but most of those do so periodically and regularly, with only a few exceptions. One of the most prominent exceptions is Betelgeuse, the red supergiant that makes up one of the “shoulders” of the constellation Orion. Over the past five years, not only has it been fluctuating in brightness, but its dimming in late 2019 and early 2020, followed by a strange brightening in 2023, indicates variation in a fashion never before witnessed by living humans.

Betelgeuse is typically the 10th brightest star in our sky, but fell out of the top 20 during its faintest in 2020 and rose as high as the 7th brightest in 2023. As a red supergiant, it’s only a matter of time before it undergoes a core-collapse supernova, although no one knows how to predict when that will occur. There’s no scientific reason to believe that Betelgeuse is in any more danger of going supernova today than at any random day over the next ~100,000 years or so, but many of us — including a great many professional and amateur astronomers — are hoping to witness the first naked-eye supernova in our galaxy since 1604. Although it won’t pose a danger to us, it will be spectacular. Here’s what we’ll be able to observe from here on Earth.

This simulation of a red supergiant’s surface, sped up to display an entire year of evolution in just a few seconds, shows how a “normal” red supergiant evolves during a relatively quiet period with no perceptible changes to its interior processes. The enormity of its surface and the volatility of the tenuous outer layers leads to tremendous variability on short but irregular timescales.

Right now, Betelgeuse is:

• absolutely enormous,
• irregularly shaped,
• and with an uneven surface temperature.

Located approximately 640 light-years away, it’s more than 2,000 °C cooler than our Sun, but also much larger, at approximately 900 times our Sun’s radius and occupying some 700,000,000 times our Sun’s volume. If you were to replace our Sun with Betelgeuse, it would engulf Mercury, Venus, Earth, Mars, the asteroid belt, and even Jupiter!

But there are also enormous, extended emissions around Betelgeuse from material that’s been blown off over the past few dozen millennia: matter and gas that extends out farther than Neptune’s orbit around our Sun. Over time, as the inevitable supernova approaches, Betelgeuse will shed more mass, continue to expand, dim-and-brighten chaotically, and will burn progressively heavier elements in its core.

The nebula of expelled matter created around Betelgeuse, which, for scale, is shown in the interior red circle. This structure, resembling flames emanating from the star, forms because the behemoth is shedding its material into space. The extended emissions go beyond the equivalent of Neptune’s orbit around the Sun. Statistically, there’s around a 1-in-4000 chance that Betelgeuse has already exploded, and we’re just awaiting the arrival of its light.

Even when it transitions to the more advanced stages of life within its core, from carbon-burning to then neon and oxygen and eventually silicon fusion, we won’t have any directly observable signatures of those events. The rate of the core’s fusion and energy output will change, but our understanding of how that affects the star’s photosphere and chromosphere — the parts that we can observe — is too poor for us to extract concrete predictions about. The energy spectrum of the neutrinos produced in the core, the one observable we know will change, will only become important during the silicon-burning stage, and even then, we’ll only have a few days, maximum, to predict the eventual supernova.

But at some critical moment in the star’s evolutionary process, the inner core’s silicon burning will reach completion, and the radiation pressure deep inside Betelgeuse will plummet. As this pressure was the only thing holding the star up against gravitational collapse, the inner core, composed of elements like iron, cobalt, and nickel, will then begin to implode.

Artist’s illustration (left) of the interior of a massive star in the final stages, pre-supernova, of silicon-burning. (Silicon-burning is where iron, nickel, and cobalt form in the core.) A Chandra image (right) of the Cassiopeia A supernova remnant today shows elements like Iron (in blue), sulphur (green), and magnesium (red). Betelgeuse is expected to follow a very similar pathway to previously observed core-collapse supernovae.

It’s difficult to imagine the scale of this: an object totaling about 20 solar masses, spread out over the volume of Jupiter’s orbit, whose inner core is comparable to (and more massive than) the size of the Sun, suddenly begins to rapidly collapse. As large as the gravitational force was pulling everything in on itself, it was counterbalanced by the radiation pressure coming from nuclear fusion in the interior. Now, that fusion (and that outward pressure) is suddenly gone, and collapse proceeds uninhibited.

The innermost atomic nuclei — a dense collection of iron, nickel, cobalt, and other similar elements — get forcefully scrunched together, where they fuse into an enormous ball of neutrons. The layers atop them also collapse, but rebound against the dense proto-neutron star in the core, which triggers an incredible burst of nuclear fusion. As the layers pile up, they rebound, creating waves of fusion, radiation, and pressure that cascade through the star.

In the inner regions of a star that undergoes a core-collapse supernova, a neutron star begins to form in the core, while the outer layers crash against it and undergo their own runaway fusion reactions. Neutrons, neutrinos, radiation, and extraordinary amounts of energy are produced, with neutrinos and antineutrinos carrying the majority of the core-collapse supernova’s energy away. Whether the remnant becomes a neutron star or black hole, ultimately, depends on how much mass remains in the core during this process.

These fusion reactions take place over an incredibly brief timescale of only approximately 10 seconds, and the overwhelming majority of the energy is carried away in the form of neutrinos, which hardly ever interact with matter. The remaining energy-carrying particles, including neutrons, nuclei, electrons, and photons, even with the intense amounts of energy imparted to them, have to have their energy cascade and propagate through the entire outer layers of the star.

As a result of this, the neutrinos become the first signals to escape, and the first signal to arrive on Earth. With the energies that supernovae impart to these particles — on the order of around ~10–50 MeV per quantum of energy — the neutrinos will move at speeds indistinguishable from the speed of light. Whenever the supernova actually occurs (or occurred, which could have been anytime from the 14th century onward), it will be the neutrinos that arrive here on Earth first, some 640 years later.

A neutrino event, identifiable by the rings of Cherenkov radiation that show up along the photomultiplier tubes lining the detector walls, showcase the successful methodology of neutrino astronomy. This image shows multiple events, and is part of the suite of experiments paving our way to a greater understanding of neutrinos. The neutrinos detected in 1987 marked the dawn of both neutrino astronomy and the rebranding of nucleon decay experiments as neutrino detector experiments.

In 1987, a supernova from 168,000 light-years away wound up creating a signal of a little over 20 neutrinos across three small neutrino detectors that were operating at the time. There are many different neutrino observatories in operation today, much larger and more sensitive than the ones we had at our disposal some 37 years ago, and Betelgeuse, just 640 light-years away only, would send a signal some 70,000 times stronger on Earth due to its close proximity.

Now, at the end of 2024, if Betelgeuse were to go supernova, our first surefire signature would come in the form of high-energy neutrinos flooding our neutrino detectors all over the world in a burst spanning some 10–15 seconds. There would literally be millions, perhaps even tens of millions, of neutrinos picked up all at once by these observatories. A few hours later, when the first energetic ripples created by this cataclysm reached the star’s outer layers, a “breakout” of photons would reach us: a swift spike that increased Betelgeuse’s optical brightness tremendously.

In 2011, one of the stars in a distant galaxy that happened to be in the field of view of NASA’s Kepler mission spontaneously and serendipitously went supernova. This marked the first time that a supernova was caught occurring in the act of transitioning from a normal star to a supernova event, with a surprising ‘breakout’ temporarily increasing the star’s brightness by a factor of about 7,000 over its previous value.

All of a sudden, the luminosity of Betelgeuse would spike by about a factor of 7,000 from its previously steady value. It would go from one of the brightest stars in the night sky to the brightness of a thin crescent Moon: about 40 times brighter than the planet Venus. That peak brightness would only last for a few minutes before falling again back to being just about 5 times brighter than it previously was, but then the traditional supernova rise begins.

Over a time period of approximately 10 days, the brightness of Betelgeuse will gradually rise, eventually becoming about as bright as the full Moon. Its brightness will surpass all the stars and planets after about an hour, will reach that of a half Moon in three days, and will reach its maximum brightness after approximately 10 days. To skywatchers across the globe, Betelgeuse will appear to be even brighter than the full Moon, as instead of being spread out over half a degree (like the full Moon), all of its brightness will be concentrated into a single, solitary, saturated point.

The constellation Orion as it would appear if Betelgeuse went supernova in the very near future. The star would shine approximately as brightly as the full Moon, but all the light would be concentrated to a point, rather than extended over a disk that covers approximately half a degree. Peak brightness should be achieved roughly two weeks after the initial explosion.

As a type II supernova, the light from an exploded Betelgeuse will remain bright for a rather long time, although there are large variations within these classes of supernovae for exactly how bright they become and how bright they remain over long periods of time. (When such an event occurs in our galaxy next, it will teach us a tremendous amount about the relationship between the progenitor star and the supernova explosion that it produces!) The supernova, after reaching maximum brightness, will slowly begin to fade over the timespan of about a month, becoming about as dim as a half Moon after 30 days time.

Over the next two months, however, its brightness will plateau, where only specialized instruments and astrophotographers will be able to detect a minuscule dimming; the typical human eye will not be able to discern a change in brightness over this time. Following that period, however, the brightness will drop precipitously and suddenly over the next (fourth) month since detonation: it will go back to barely being brighter than Venus by the end of that time. And finally, over the next year or two, it will gradually fade out of existence, with the supernova remnant visible only through telescopes.

Type II supernovae vary between different sub-types and individual events, but obey the same general curve, with a rise lasting approximately 10 days, a short fall-off lasting a month, a plateau lasting another two months, a steep drop lasting a month, and then a gradual fade-out lasting a year or longer.

At peak brightness, Betelgeuse will shine approximately as brightly as 10 billion Suns all packed together; by the time a couple of years have gone by, it will be too faint to be seen with the naked human eye. The reason the supernova remains so bright for the first three months or so isn’t even from the explosion itself, but rather from a combination of radioactive decays (from cobalt, for example) and the expanding gases in the supernova remnant.

During those first three months or so, Betelgeuse will be so bright that it will be clearly visible during the day as well as the night; only after the fourth month or so will it become a nighttime-only object. And as it begins to fade from its brightness to look like a normal star once again, the extended structures should remain illuminated through a telescope for decades, centuries, and even millennia to come. It will become the closest supernova remnant in recorded history, and will remain a spectacular sight (and astronomical object of study) for generations to come.

This image shows the supernova remnant of SN 1987A in six different wavelengths of light. Even though it’s been 37 years since this explosion occurred, and even though it’s right here in our own backyard, the material around the central engine has not cleared enough to expose the stellar remnant. For contrast, Cow-like objects (also known as fast blue optical transients) have their cores exposed almost immediately.

Whenever Betelgeuse (or a similarly close red supergiant) finally does go supernova — and it could be tonight, next decade, or 100,000 years from now — it will become the most-witnessed astronomical event in human history, visible to nearly all of Earth’s inhabitants. The first signal to arrive won’t be visual at all, but will come in the form of neutrinos, a typically elusive particle that will flood our terrestrial detectors by the millions.

After that, a few hours later, the light will first arrive in a spike, followed by a gradual brightening over a little more than a week, which will fall off in stages over the coming months before gradually declining for years. The remnant, which consists of gaseous outer layers illuminated for thousands of years, will continue to delight our descendants for generations to come. We have no idea when the show will begin, but at least we know what to look for and expect when it actually occurs!