Chondrules are spherical or subspherical particles of crystallized or partially crystallized liquid silicates that constitute large-volume fractions of most chondritic meteorites. Chondrules typically range \(0.1-2\,\) mm in size and solidified with cooling rates of \(10-1000\,\mathrm{K\,h^{-1}}\) , yet these characteristics prove difficult to reconcile with proposed formation models. We numerically show that collisions among planetesimals containing volatile materials naturally explain both the sizes and cooling rates of chondrules. We show that the high-velocity collisions with volatile-rich planetesimals first induced in the solar nebula by Jupiter’s formation produced increasing amounts of silicate melt for increasing impact velocities above \(2\,\mathrm{km\,s^{-1}}\) . We propose that the expanding gas formed from volatile materials by collisional heating dispersed and cooled the silicate melt, resulting in droplet sizes and cooling rates consistent with the observed sizes and inferred cooling rates. We further show that the peak melt production is linked to the onset of Jupiter’s runaway gas accretion, and argue that the peak age of chondrules points to Jupiter’s birth dating 1.8 Myr after CAIs.
