Quark star collisions typically eject large amounts of matter both along the equatorial plane and toward the poles. The basic units of this ejecta are initially “quark nuggets” of varying sizes. Over time, these nuggets undergo two competing processes: evaporation, in which protons or neutrons escape (similar to water molecules evaporating), and absorption, in which external protons and neutrons are captured by the nuggets. The efficiency of evaporation depends mainly on the binding energy of quark matter and the temperature. In the dense environment following a quark star merger, evaporation and absorption may reach equilibrium, suppressing net evaporation. As the ejecta expand and cool, both evaporation and absorption rates eventually drop to very low levels, and the composition of the ejecta effectively freezes. Rigorous calculations show that, across a wide parameter space (the binding energy of quark matter and the temperature and density evolution trajectory), these quark nuggets cannot efficiently evaporate into free neutrons and protons but instead remain bound as quark nuggets. This finding carries significant observational implications: if the merger products are dominated by quark nuggets, the environment would lack sufficient free neutrons to trigger rapid neutron capture (r-process) nucleosynthesis, which in turn means that heavy elements necessary to power a kilonova would not be produced. In other words, if quark stars do exist in the universe, their mergers may not light up a kilonova in the way neutron star mergers do. Future observations of kilonovae therefore hold great promise: not only could they provide critical constraints on the binding energy of quark matter, but they may also serve as decisive evidence for or against the very existence of quark stars.