Fusion Keeps the Star Stable
Inside massive stars, hydrogen fuses to form helium. Energy released from these reactions, in the form of gamma rays, heats up the surrounding star matter, pushing it outward. This pressure counterbalances gravity [1], which tries to suck the star back in. As a result, the star remains stable—for a while._
Mass Creates Unusual Circumstances
In most stars, gravity wins. The star runs out of atoms to fuse and can’t generate enough energy to push back. It collapses into either a black hole or a neutron star, and its shell explodes. But supernova 2006GY was so huge and stayed bright for so long that something else must have happened while it died.
Pair Production Saps Energy
One explanation, the so-called pair-instability model, requires an extremely massive, hot star. Once the core temperature hits 1.8 billion degrees Fahrenheit, the gamma rays born from nuclear fusion in the core spontaneously morph into pairs of electrons and their antimatter twins, positrons [2].
A Thermonuclear Ending
Now the gamma rays that previously counterbalanced gravity’s inward pull no longer exist. Gravity compresses the star [3], transforming the core into heavy elements like iron and nickel. Once the core gets to about 5.4 billion degrees, a runaway thermonuclear reaction [4] blows the star apart, leaving nothing behind.
How We Find Them
Canvass the Sky
California Institute of Technology astronomer Robert Quimby, who found the two brightest supernovae on record, including 2006GY, scans large areas of the sky nightly with a robotic telescope. His search program compares snapshots of the sky on previous nights—essentially looking for bright spots that weren’t there before.
Don’t Skip the Core
Most supernova hunters neglect to search the cores of galaxies or the areas around massive black holes, because these locales can often turn up too many false alarms. Yet that’s exactly where Quimby spotted his bright light; he decided to peek in there precisely because no one else was doing so.
Use Lots of Eyes
Quimby alerted other astronomers to his potential find. Within a month, astrophysicist Nathan Smith of the University of California at Berkeley was leading a team using a variety of observatories to gather added optical and spectral data. They also used the Chandra X-ray Observatory to measure 2006GY’s x-ray emissions. To see more shots of the hypernova and answers to frequently asked questions, launch the gallery here.
