Stellar grandeur carries penalties. Although the most massive stars possess enormous fuel reserves, their fierce energy output can exhaust those reserves far faster than the Sun consumes its smaller supply. Brilliance buys little time. Their lives expose an astronomical irony: the stars that seem most extravagantly supplied are often those least able to make their inheritance last.
Size can mislead badly. Betelgeuse, a red supergiant whose radius spans hundreds of solar radii, has expanded into a swollen envelope rather than simply becoming an exceptionally heavy version of the Sun. Mass tells another story. R136a1, in the Large Magellanic Cloud, is estimated to contain well over one hundred solar masses, although its precise mass depends on models and observations. The distinction matters here. A ranking by diameter therefore answers a different question from a ranking by mass, and neither measurement alone explains how a star will die.
Their deaths resist neatness. Nuclear fusion builds heavier elements inside massive stars, but once an iron core can no longer support itself, core collapse can set off a supernova and leave a neutron star or black hole. Some endings stay dark. Depending on its structure and mass loss, a star may instead collapse into a black hole without producing a bright explosion, complicating the census of stellar deaths. Their debris outlasts them. Expelled material supplies later generations of stars and planets with heavier elements; against that inheritance, even the largest surviving star is only a temporary concentration of borrowed matter.
