All stars balance gravity with pressure. As light elements such as hydrogen fuse in a star’s core, the reactions generate photons that press outward, counteracting the pull of gravity. In larger stars, pressure at the core is high enough to fuse heavier elements such as oxygen and carbon, creating more photons. But in stars bigger than 100 solar masses or so, there’s a hitch. When oxygen ions begin to fuse with one another, the reaction releases photons that are so energetic, they spontaneously transmute into electron-positron pairs. With no photons, there’s no outward pressure—and the star begins
One of two things can happen next. The collapse can create even more pressure, reigniting enough oxygen to create a burst of energy. This burst is enough to toss off the outer layers of the star but not enough to create a full supernova. The cycle can repeat itself in pulses—astronomers call this case a “pulsational” pair-instability supernova—until the star loses enough mass to end its life in an ordinary supernova. A team led by the California Institute of Technology’s Robert M. Quimby announced it had identified one of these and has submitted a paper for publication.