Laboratory Modeling of Supernova Remnants Collisions: Implications for Triggered Star Formation

Abstract Theoretical models of star formation consistently underestimate the rates observed in astronomical surveys. Stars form within giant molecular clouds, which fragment into dense clumps under the combined influences of turbulence, magnetic fields, radiation, and gravity. While some of these clumps collapse spontaneously, others require an external trigger, a mechanism estimated to account for 14%–25% of star formation in regions such as the Elephant Trunk Nebula. Laboratory astrophysics has emerged as a powerful approach for investigating such triggering processes, in particular those involving supernova remnants (SNRs). Recent experiments, guided by well-established scaling laws, have successfully replicated the dynamics of SNRs and their interactions with dense clumps or other SNRs. In this work, we present a comprehensive numerical study of these experimental configurations using the 3D radiation-hydrodynamics code TROLL. The simulations provide enhanced insight into the underlying physical mechanisms, accurately reproduce key experimental phenomena, and offer valuable comparisons with analytical models. This study underscores the strong synergy between laboratory experiments and numerical simulations, laying a robust foundation for future advancements in laboratory astrophysics. Furthermore, we propose a new experimental setup that offers improved scaling for the asymmetric collision observed in the DEM L316 system. Our findings also show that SNR collisions in dense environments can decrease the gravitational stability of dense clumps, thereby promoting their collapse and potentially triggering star formation.