ALMA (ESO/NAOJ/NRAO)/Alexandra Angelich (NRAO/AUI/NSF)
Ian Shelton was alone at a telescope in the remote Atacama Desert of Chile. He had spent three hours taking a picture of the Large Magellanic Cloud. This wispy galaxy orbits our own, the Milky Way. Suddenly, Shelton was plunged into darkness. High winds had taken hold of the rolltop door in the observatory’s roof, slamming it shut.
“This was maybe telling me I should just call it a night,” recalls Shelton. It was February 23, 1987. And that evening, Shelton was the telescope operator at Las Campanas Observatory.
He grabbed an 8-by-10 inch glass plate from the telescope’s camera. It had caught an image of the night sky. But it was only a negative. So Shelton headed off to the darkroom. (Back then, photographs had to be developed by hand from negatives instead of appearing instantly on a screen.) As a quick quality check, the astronomer compared the just-developed picture with one he had taken the night before.
And one star caught his eye. It hadn’t been there the previous night. “This is too good to be true,” he thought. But to be sure, he stepped outside and looked up. And there it was — a faint point of light that wasn’t supposed to be there.
He walked down the road to another telescope. There, he asked astronomers what they could say about an object that bright appearing in the Large Magellanic Cloud, just outside the Milky Way.
“Supernova!” was their response. Shelton ran outside with the others to double-check with their own eyes. In the group was Oscar Duhalde. He saw the same thing earlier that evening.
They were witnessing the explosion of a star. This supernova was the closest seen in nearly four centuries. And it was bright enough to view without a telescope.
“People thought they’d never see this in their lifetime,” recalls George Sonneborn. He is an astrophysicist at NASA’s Goddard Space Flight Center in Greenbelt, Md. (NASA is short for the National Aeronautics and Space Administration.)
With roughly 2 trillion galaxies in the observable universe, there’s almost always a star exploding somewhere. But a supernova close enough to be seen with the unaided eye is rare. In the Milky Way, astronomers estimate, a supernova goes off every 30 to 50 years. But until that time, the most recent one seen was in 1604. At a distance of about 166,000 light-years, the new one was the closest since the time of Galileo. Astronomers would dub it SN (for supernova) 1987A (indicating it was the first of that year).
Supernovas are “important agents of change in the universe,” notes Adam Burrows. He is an astrophysicist at Princeton University in New Jersey. Most heavyweight stars end their lives as supernovas.
These explosive events also may trigger the birth of new ones. Such cataclysms can change the fate of entire galaxies by stirring up the gas needed to build more stars. Most chemical elements heavier than iron, perhaps even all of them, are forged in the chaos of such explosions. Lighter elements are created over a star’s lifetime and then spewed into space to seed a new generation of stars and planets — and life. These include “the calcium in your bones, the oxygen you breathe, the iron in your hemoglobin,” Burrows explains.
Thirty years after its discovery, supernova 1987A remains a celebrity. It was the first supernova for which the original star could be identified. And it spewed the first neutrinos — a kind of particle smaller than an atom — detected from beyond the solar system. Those subatomic particles confirmed decades-old theories about what happens in the heart of an exploding star.
Today, the supernova’s story continues to be written. New observatories draw out more details as shock waves from the explosion keep plowing through the gas between stars.
SN 1987A has dimmed “by a factor of 10 million,” notes Robert Kirshner. “But we can still study it.” An astrophysicist, Kirshner works at the Harvard-Smithsonian Center for Astrophysics in Cambridge, Mass. In fact, he notes, today “We can study it better and over a wider range of light than we could in 1987.”
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A daily adventure
Communication was a bit slower when 1987A exploded. Shelton’s attempts to call the International Astronomical Union, or IAU, in Cambridge, Mass., failed. So a driver took off to La Serena, a town some 100 kilometers (62 miles) away. From there a telegram was dispatched to share the unexpected news with the IAU. (Before the internet, telegrams were how people quickly sent written messages long distances.)
At first, there were doubters. “I thought, that’s got to be a joke,” says Stan Woosley. He is an astrophysicist at the University of California, Santa Cruz. But as word spread via telegram and telephone, it quickly became clear this was no prank. Amateur astronomer Albert Jones in New Zealand reported seeing the supernova the same night — until clouds moved in. About 14 hours after the discovery, NASA’s International Ultraviolet Explorer satellite was watching it. Astronomers around the world scrambled to redirect telescopes both on the ground and in space.
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Telegram announces 1987A
Ian Shelton sent a telegram announcing the discovery of SN 1987A, a supernova that can be seen here after the explosion (right) but not before (left). Images: ESO
“The whole world got excited,” Woosley remembers. “It was a daily adventure. There was always something coming in.” At first, astronomers suspected that 1987A was a type 1a supernova. This results from the detonation of a stellar core — one that is left behind after a star like the sun quietly sheds gas at the end of its life. But it soon became clear 1987A was a type 2 supernova. It was the explosion of a star many times heavier than our sun.
Observations taken the next day in Chile and South Africa showed hydrogen gas hurtling away from the explosion at roughly 30,000 kilometers (19,000 miles) per second. That’s about one-tenth the speed of light. After the initial flash, the supernova faded for about a week but then resumed brightening for about 100 days. It eventually maxed out shining with the light of roughly 250 million suns!
The right track
Since first spotted, SN 1987A has provided several surprises. But it didn’t lead to a fundamental shift in how astronomers think about these explosions, says David Arnett. He is an astrophysicist at the University of Arizona in Tucson. The general idea is that a type 2 supernova goes off when a heavyweight star runs out of fuel and can no longer support its own weight. This had been suspected for decades. It was largely confirmed by 1987A.
Stars live in a delicate balance between gravity and gas pressure. Gravity wants to crush a star. High temperatures and extreme densities in the center of a star allow the nuclei of hydrogen atoms to slam together. This creates helium and frees lots of energy. That energy pumps up the pressure and keeps gravity in check.
Once a star’s core runs out of hydrogen, it begins fusing helium into atoms of carbon, oxygen and nitrogen. And for stars like the sun, that’s about as far as they get.
But if a star is more than about eight times as massive as our sun, it can go on to forge even heavier elements. All that weight on the core keeps the pressure and temperature extremely high. The star forges heavier and heavier elements until iron is created. Iron is not a stellar fuel. Fusing it with other atoms doesn’t release energy. In fact, iron saps energy from its surroundings.
Without an energy source to fight against gravity, the bulk of the star now comes crashing down on its core. That core collapses on itself until it becomes a ball of neutrons. That ball can survive as a neutron star — a hot orb now only about the size of a city. But if enough gas from the dying star rains down on the core, the neutron star loses its own battle with gravity. What results is a black hole.
Before that happens, the initial onrush of gas from the rest of the star hits the core and bounces back outward. This sends a shock wave back toward the surface, which tears the star apart. The ensuing explosion can forge elements even heavier than iron. More than half of the periodic table of elements may have been formed by supernovas.
Newly formed elements aren’t the only things a supernova spits out. Neutrinos are too. These nearly massless subatomic particles barely interact with matter.
Theorists had predicted that neutrinos should be released during the collapse of a star’s core — and in huge amounts. Despite their ghostly nature, neutrinos are suspected of being the main driving force behind the supernova. They are thought to inject energy into the developing shock wave. A lot of energy. They may, in fact, account for 99 percent of the energy released in such an explosion.
Neutrinos can pass through the bulk of the star unimpeded. That means they can get a head start out of the star, eventually arriving at Earth before the blast of light.
Confirmation of this prediction was one of the big successes from 1987A. Three neutrino detectors on different continents registered a nearly simultaneous uptick in neutrinos roughly three hours before Shelton recorded the flash of light. A detector in Japan counted 12 neutrinos. Another in Ohio detected eight. A facility in Russia detected five more. In all, 25 neutrinos turned up. That counts as a deluge in neutrino science.
“That was huge,” agrees Sean Couch. He is an astrophysicist at Michigan State University in East Lansing. “That told us beyond a shadow of a doubt that a neutron star formed and radiated neutrinos.”
While the neutrinos were expected, the type of star that “went supernova” was not. Before 1987A, astronomers thought that only puffy red stars known as red supergiants would end their lives in a supernova. These are gargantuan stars. One nearby example: the bright star Betelgeuse in the constellation Orion. It is at least as wide as the orbit of Mars. But the star that exploded as 1987A had been a blue supergiant. Known as Sanduleak -69° 202, it was hotter and more compact than a red supergiant. Clearly, 1987A didn’t fit the mold.
“SN 1987A taught us that we did not know everything,” Kirshner says.
A necklace of pearls
More surprises emerged after the launch of the Hubble Space Telescope three years later. Its early images were fuzzy. The reason was a now infamous defect in the telescope’s main mirror. Once corrective optics were installed in 1993, unexpected details of the fading explosion came into focus.
“Those first pictures from Hubble were jaw-dropping,” says Shelton, who is now a teacher in the Toronto, Canada, area. A thin ring of glowing gas could be faintly seen in earlier images from the ground. Now, it encircled the site like a Hula-Hoop. Above and below that ring were two fainter rings. This trio formed an hourglass shape.
“No other supernova had shown that kind of phenomenon,” says Richard McCray. He is an astrophysicist at the University of California, Berkeley. It is not because it doesn’t happen, he points out. No, it’s because other supernovas were too far away to be seen so well.
The central ring spanned 1.3 light-years across and was expanding at about 37,000 kilometers (23,000 miles) per hour. The ring’s size and how quickly it was growing indicated that the star dumped a lot of gas into space about 20,000 years before it exploded. That could explain why Sanduleak -69 202 was a blue supergiant when it exploded. Some type of earlier outburst might have whittled the star down to expose hotter — and therefore bluer — layers.
One leading idea for how the rings formed is that this star might be the offspring of two that once, long ago, locked into an orbit around one another. Eventually that stellar pair spiraled into each other. As they merged, some excess gas might have been expelled, forming a ring that aligned with the original orbit. Other gas may have funneled in the perpendicular direction. Rapid rotation of a single star or powerful magnetic fields also might have directed gas from an eruption into a loop around the star.
The primary ring has gotten only more intriguing with time. In 1994, a bright spot appeared on the ring. A few years later, three more spots emerged. By January 2003, the entire ring had lit up with 30 hot spots. All were drifting away from the center of the explosion. “It was like a necklace of pearls,” Kirshner says — “a really beautiful thing.” A shock wave from the supernova had caught up with the ring and started to heat up clumps of gas.
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By now, the hot spots are fading as new ones are showing up outside the ring. Given how quickly the spots are waning, the ring will probably disintegrate sometime in the next decade. “In a way, this is the end of the beginning,” Kirshner concludes.
The elusive neutron star
One of the enduring mysteries of 1987A is what became of the neutron star that formed at the heart of the explosion. “It’s a cliffhanger,” Kirshner says. “Everybody thinks that the neutrino signal means that a neutron star formed.” But there’s still no sign of it, despite three decades of searching with many different types of telescopes.
“It’s a bit embarrassing,” Burrows admits. Astronomers haven’t been able to find the pinprick of light from a glowing orb in the middle of the debris. There is no steady pulse from a pulsar. That’s a rapidly spinning neutron star, which sweeping out beams of radiation like a cosmic lighthouse. Nor is there any hint of heat radiated by dust clouds exposed to the harsh light of a hidden neutron star. Finding that neutron star “is one of the things most crucial to closing the chapter on 87A,” says Burrows. “We need to know what was left.”
The neutron star is probably there, researchers say. Today, however, it may be too feeble to see. Or perhaps it was short-lived. If more material rained down after the explosion, the neutron star could have gained too much weight. Then it might have collapsed under its own gravity to form a black hole. Right now, there’s no way to tell.
Answers to this mystery and others will depend on new and future telescopes. As technology advances, new facilities keep providing fresh looks at the remains of 1987A. Chile’s Atacama Large Millimeter/submillimeter Array, or ALMA, now combines the power of 66 radio-telescope dishes. In 2012, it used 20 antennas to peer into the heart of the explosion’s debris. ALMA is sensitive to electromagnetic waves that can penetrate clouds of debris surrounding the supernova site. “That gives us a look at the guts of the explosion,” McCray says.
Within those guts lurk solid grains of carbon- and silicon-based chemicals, researchers reported in 2014. These would have formed in the supernova’s wake. Such dust grains are important ingredients for making planets, astronomers believe. Supernova 1987A appears to be creating a lot of this dust. That suggests that stellar explosions play a crucial role in seeding the cosmos with planet-building material. Whether that dust survives shock waves that are still ricocheting around the leftovers of the supernova is still unknown.
From Earth, the universe can seem unchanging. But over the past 30 years, 1987A has shown us cosmic change on a human timescale. A star was destroyed. New elements formed. And a tiny corner of the cosmos was altered forever. As the closest supernova seen in 383 years, 1987A gave people an intimate glimpse of one of the most fundamental and powerful drivers of evolution in the universe.
“It was a long time coming,” Shelton says. “This particular supernova … deserves all the accolades it gets.” But even though 1987A was close, he adds, it was still outside the Milky Way. He and others are waiting for one to go off within our galaxy. “We’re overdue for a bright one here.”
(for more about Power Words, click here)
agent A compound or activating form of energy (such as light or other types of radiation) that has a role to play in getting something done.
amateur One who engages in a pursuit as a pastime, and not as a profession.
antenna (in physics) Devices for picking up (receiving) electromagnetic energy. (plural: antennae)
array A broad and organized group of objects. Sometimes they are instruments placed in a systematic fashion to collect information in a coordinated way.
astrophysics An area of astronomy that deals with understanding the physical nature of stars and other objects in space. People who work in this field are known as astrophysicists.
atom The basic unit of a chemical element. Atoms are made up of a dense nucleus that contains positively charged protons and neutrally charged neutrons. The nucleus is orbited by a cloud of negatively charged electrons.
atomic Having to do with atoms, the smallest possible unit that makes up a chemical element.
black hole A region of space having a gravitational field so intense that no matter or radiation (including light) can escape.
calcium A chemical element which is common in minerals within Earth’s crust.
carbon The chemical element having the atomic number 6. It is the physical basis of all life on Earth. Carbon exists freely as graphite and diamond.
chemical A substance formed from two or more atoms that unite (become bonded together) in a fixed proportion and structure.
cloud A plume of molecules or particles, such as water droplets, that move under the action of an outside force, such as wind, radiation or water currents.
compound (often used as a synonym for chemical) A compound is a substance formed from two or more chemical elements united in fixed proportions.
constellation Patterns formed by prominent stars that lie close to each other in the night sky. Modern astronomers divide the sky into 88 constellations, 12 of which (known as the zodiac) lie along the sun’s path through the sky over the course of a year.
cosmic An adjective that refers to the cosmos — the universe and everything within it.
debris Scattered fragments, typically of trash or of something that has been destroyed.
density The measure how condensed an object is, found by dividing the mass by the volume.
electromagnetic waves Energy that travels as a wave, including forms of light. Electromagnetic radiation is typically classified by its wavelength. The spectrum of electromagnetic radiation ranges from radio waves to gamma rays. It also includes microwaves and visible light.
element (in chemistry) Each of more than one hundred substances for which the smallest unit of each is a single atom. Examples include hydrogen, oxygen, carbon, lithium and uranium.
evolution (v. to evolve) A process by which species undergo changes over time, usually through genetic variation and natural selection. Or the term can refer to changes that occur as some natural progression within the non-living world (such as computer chips evolving to smaller devices which operate at an ever faster speed).
factor Something that plays a role in a particular condition or event; a contributor.
field (in physics) A region in space where certain physical effects operate, such as magnetism (created by a magnetic field), gravity (by a gravitational field), mass (by a Higgs field) or electricity (by an electrical field).
force Some outside influence that can change the motion of a body, hold bodies close to one another, or produce motion or stress in a stationary body.
forge (noun) A furnace or shop where metal is worked and turned into new materials. (verb) To shape metals under heat and/or pressure, or (colloquially) to form one element from another under the intense heat and pressure inside stars.
fundamental Something that is basic or serves as the foundation for another thing or idea.
galaxy A massive group of stars bound together by gravity. Galaxies, which each typically include between 10 million and 100 trillion stars, also include clouds of gas, dust and the remnants of exploded stars.
gravity The force that attracts anything with mass, or bulk, toward any other thing with mass. The more mass that something has, the greater its gravity.
helium An inert gas that is the lightest member of the noble gas series. Helium can become a solid at -272 degrees Celsius (-458 degrees Fahrenheit).
hemoglobin A molecule that binds to oxygen in the blood, carrying it around to tissues.
hydrogen The lightest element in the universe. As a gas, it is colorless, odorless and highly flammable. It’s an integral part of many fuels, fats and chemicals that make up living tissues.
iron A metallic element that is common within minerals in Earth’s crust and in its hot core. This metal also is found in cosmic dust, and in many meteorites.
light-year The distance light travels in one year, about 9.48 trillion kilometers (almost 6 trillion miles).
magnetic field An area of influence created by certain materials, called magnets, or by the movement of electric charges.
Mars The fourth planet from the sun, just one planet out from Earth.
mass A number that shows how much an object resists speeding up and slowing down — basically a measure of how much matter that object is made from.
matter Something which occupies space and has mass.
Milky Way The galaxy in which Earth’s solar system resides.
NASA Short for the National Aeronautics and Space Administration. Created in 1958, this U.S. agency quickly became a leader in space research and in stimulating public interest in space exploration.
neutrino A subatomic particle with a mass close to zero. Neutrinos rarely react with normal matter.
neutron A type of particle found in the nucleus of all atoms except hydrogen. Having no electric charge, it has a mass slightly greater than that of a proton.
neutron star The very dense corpse of what had once been a star with a mass four to eight times that of our sun. As the star died in a supernova explosion, its outer layers shot out into space. Its core then collapsed under its intense gravity, causing protons and electrons in its atoms to fuse into neutrons (hence the star’s name). Astronomers believe neutron stars form when large stars undergo a supernova but aren’t massive enough to form a black hole. A single teaspoonful of a neutron star, on Earth, would weigh a billion tons.
New Zealand An island nation in the southwest Pacific Ocean, east of Australia.
nitrogen A colorless, odorless and nonreactive gaseous element that forms about 78 percent of Earth's atmosphere. Its scientific symbol is N.
nucleus (in physics) The central core of an atom, containing most of its mass.
observatory (in astronomy) The building or structure (such as a satellite) that houses one or more telescopes.
optics Having to do with vision or what can be seen.
orbit The curved path of a celestial object or spacecraft around a star, planet or moon.
oxygen A gas that makes up about 21 percent of Earth’s atmosphere.
perpendicular An adjective that describes two things that are situated approximately 90 degrees to each other. In the letter “T,” the top line of the letter is perpendicular to the bottom line.
phenomenon Something that is surprising or unusual.
planet A celestial object that orbits a star, is big enough for gravity to have squashed it into a roundish ball and that must have cleared other objects out of its orbital neighborhood.
pressure Force applied uniformly over a surface, measured as force per unit of area.
primary An adjective meaning major, first or most important.
pulsar The name for a spinning, ultra-dense neutron star. When these stars rotate, they emit short, regular pulses of radio waves or X-rays (and occasionally both at alternate intervals).
radiation (in physics) One of the three major ways that energy is transferred. It uses electromagnetic waves to carry energy from one place to another. Unlike conduction and convection, radiation can transfer energy across empty space.
radio Waves in a part of the electromagnetic spectrum; they are a type that people now use for long-distance communication. Longer than the waves of visible light, radio waves are used to transmit radio and television signals; it is also used in radar.
red supergiant A very large star that develops after helium-fueled fusion reactions have ceased in the core of a very massive star (a star more than 15 times the mass of our sun).
satellite A moon orbiting a planet or a vehicle or other manufactured object that orbits some celestial body in space.
shock waves Tiny regions in a gas or fluid where properties of the host material change dramatically owing to the passage of some object (which could be a plane in air or merely bubbles in water). Across a shock wave, a region’s pressure, temperature and density spike briefly, and almost instantaneously.
silicon A nonmetal, semiconducting element used in making electronic circuits.
solar system The eight major planets and their moons in orbit around our sun, together with smaller bodies in the form of dwarf planets, asteroids, meteoroids and comets.
speed of light A constant often used in physics, corresponding to 1.08 billion kilometers (671 million miles) per hour.
star The basic building block from which galaxies are made. Stars develop when gravity compacts clouds of gas. When they become dense enough to sustain nuclear-fusion reactions, stars will emit light and sometimes other forms of electromagnetic radiation. The sun is our closest star.
stellar An adjective that means of or relating to stars.
subatomic Anything smaller than an atom, which is the smallest bit of matter that has all the properties of whatever chemical element it is (like hydrogen, iron or calcium).
sun The star at the center of Earth’s solar system. It’s an average size star about 26,000 light-years from the center of the Milky Way galaxy. The term can also be applied to a sunlike star.
supernova (plural: supernovae or supernovas) A massive star that suddenly increases greatly in brightness because of a catastrophic explosion that ejects most of its mass.
telescope Usually a light-collecting instrument that makes distant objects appear nearer through the use of lenses or a combination of curved mirrors and lenses. Some, however, collect radio emissions (energy from a different portion of the electromagnetic spectrum) through a network of antennas.
theorist A scientist whose work relies on mathematical analyses and computer models of events and physical objects or phenomena — not on experiments that test situations in the real world or that use testing and observations to collect data.
trillion A number representing a million million — or 1,000,000,000,000 — of something.
type 1 supernova A supernova that results from some binary (paired) star systems in which a white dwarf star gains matter from a companion. The white dwarf eventually gains so much mass that it explodes.
type 2 supernova This occurs when nuclear fusion can no longer continue in the core of a massive star because the core has burned through its fuel (and in the process created new elements, via fusion).
ultraviolet A portion of the light spectrum that is close to violet but invisible to the human eye.
universe The entire cosmos: All things that exist throughout space and time.
wake An area of disturbed air or water left behind an object (such as a boat or animal) moving through it.
wane To diminish gradually in size or intensity.
wave A disturbance or variation that travels through space and matter in a regular, oscillating fashion.
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Journal: W. Kunkel et al. Supernova 1987a in the Large Magellanic Cloud. International Astronomical Union Circular. No. 4316, February 24, 1987.
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