This Chandra X-ray photograph shows Cassiopeia A (Cas A, for short), the youngest supernova remnant in the Milky Way.
Credit: NASA/CXC/MIT/UMass Amherst/M.D.Stage et al.
A blindingly bright star bursts into view in a corner of the night sky — it wasn't there just a few hours ago, but now it burns like a beacon.
That bright star isn't actually a star, at least not anymore. The brilliant point of light is the explosion of a star that has reached the end of its life, otherwise known as a supernova.
Supernovas can briefly outshine entire galaxies and radiate more energy than our sun will in its entire lifetime. They're also the primary source of heavy elements in the universe. According to NASA, supernovae are “the largest explosion that takes place in space.”
On average, a supernova will occur about once every 50 years in a galaxy the size of the Milky Way. Put another way, a star explodes every second or so somewhere in the universe, and some of those aren’t too far from Earth. About 10 million years ago, a cluster of supernovae created the “Local Bubble,” a 300-light-year long, peanut-shaped bubble of gas in the interstellar medium that surrounds the solar system.
Exactly how a star dies depends in part on its mass. Our sun, for example, doesn't have enough mass to explode as a supernova (though the news for Earth still isn't good, because once the sun runs out of its nuclear fuel, perhaps in a couple billion years, it will swell into a red giant that will likely vaporize our world, before gradually cooling into a white dwarf). But with the right amount of mass, a star can burn out in a fiery explosion.
A star can go supernova in one of two ways:
- Type I supernova: star accumulates matter from a nearby neighbor until a runaway nuclear reaction ignites.
- Type II supernova: star runs out of nuclear fuel and collapses under its own gravity.
Type II supernovae
Let's look at the more exciting Type II first. For a star to explode as a Type II supernova, it must be at several times more massive than the sun (estimates run from eight to 15 solar masses). Like the sun, it will eventually run out of hydrogen and then helium fuel at its core. However, it will have enough mass and pressure to fuse carbon. Here's what happens next:
- Gradually heavier elements build up at the center, and it becomes layered like an onion, with elements becoming lighter towards the outside of the star.
- Once the star's core surpasses a certain mass (the Chandrasekhar limit), the star begins to implode (for this reason, these supernovae are also known as core-collapse supernovas).
- The core heats up and becomes denser.
- Eventually the implosion bounces back off the core, expelling the stellar material into space, forming the supernova.
What's left is an ultradense object called a neutron star, a city-sized object that can pack the mass of the sun in a small space.
There are sub-categories of Type II supernovas, classified based on their light curves. The light of Type II-L supernovas declines steadily after the explosion, while Type II-P's light stays steady for a time before diminishing. Both types have the signature of hydrogen in their spectra.
Stars much more massive than the sun (around 20 to 30 solar masses) might not explode as a supernova, astronomers think. Instead they collapse to form black holes.
Type I supernovae
Type 1 supernovae lack a hydrogen signature in their light spectra.
Type Ia supernovae are generally thought to originate from white dwarf stars in a close binary system. As the gas of the companion star accumulates onto the white dwarf, the white dwarf is progressively compressed, and eventually sets off a runaway nuclear reaction inside that eventually leads to a cataclysmic supernova outburst.
Type 1b and 1c supernovas also undergo core-collapse just as Type II supernovas do, but they have lost most of their outer hydrogen envelopes. In 2014, scientists detected the faint, hard-to-locate companion star to a Type 1b supernova. The search consumed two decades, as the companion star shone much fainter than the bright supernova.
Recent studies have found that supernovas vibrate like giant speakers and emit an audible hum before exploding.
In 2008, scientists caught a supernova in the act of exploding for the first time. While peering at her computer screen, astronomer Alicia Soderberg expected to see the small glowing smudge of a month-old supernova. But what she and her colleague saw instead was a strange, extremely bright, five-minute burst of X-rays.
With that observation, they became the first astronomers to catch a star in the act of exploding. The new supernova was dubbed SN 2008D. Further study has shown that the supernova had some unusual properties.
"Our observations and modeling show this to be a rather unusual event, to be better understood in terms of an object lying at the boundary between normal supernovae and gamma-ray bursts," Paolo Mazzali, an Italian astrophysicist at the Padova Observatory and Max-Planck Institute for Astrophysics, told Space.com in a 2008 interview.
Additional reporting by Nola Taylor Redd, Space.com Contributor
- In the journal Science, astronomers discuss "The Metamorphosis of Supernova SN 2008D."
- In Astronomy & Astrophysics, astronomers collaborated on an article, "Constraints on High-Energy Neutrino Emission From SN 2008D."
- A 2008 NASA press release announces the observation of the supernova.