Over an incredibly long timescale, the Sun’s white dwarf remnant could cool enough to become a black dwarf, a theoretical stellar remnant that emits no light. Although speculative, theoretical models give us insight into the lifespan of the Sun as a white dwarf. After transitioning into a white dwarf, the Sun is expected to cool and fade over an extraordinarily long period. It is theorized that, eventually, it will become a black dwarf — a cold, dark stellar remnant that no longer emits significant heat or light. This transformation could take place sometime after 1 quadrillion years — that’s 1,000 sets of a trillion years! Moreover, some estimates extend this timeline by a factor of up to 37, pushing the boundaries of our understanding of stellar evolution and the future of the cosmos. The eventual cessation of white dwarf stars, including our Sun, represents one of the universe’s far future events. However, these estimates are highly speculative, reliant on theoretical models of stellar cooling that project far beyond our current empirical observations. Given that the universe itself is not yet old enough for any black dwarfs to exist, this prediction is rooted more in our extrapolation of physical laws than in direct evidence.