A radiative shock (RS) is one in which the density and temperature structures are affected by radiation from the shock-heated matter. In most astrophysical shocks, the temperature and density conditions lead to strong emission, with radiation thus playing a major role therein. In particular, RS exists in the blast waves of core-collapse supernovae (CCSNe), where the radiation pressure in matter is larger than the thermal one.
Here, we present experiments to reproduce the characteristics of CCSNe with different stellar masses and initial explosion energies in a laboratory. In these experiments, shocks are driven on the SGIII prototype laser facility. We get the necessary parameters for the first time to scale with CCSNe cases using relevant scaling laws. Furthermore, the rescaled theoretical values are similar to three CCSNe cases. Based on the laboratory conditions, the driving mechanism of the supernova explosions could be investigated and unified by multiple cases.
As a further step, we conducted a study on the scaling relationship between the movement speed of the emission brightness peak, the spatial distribution of emission in the observational images of the ancient star, and the laboratory data. We found that the laboratory data can be brought into agreement with the observational images through scaling laws. This represents a valuable exploration of how laboratory radiative shock studies can help reveal the underlying patterns of supernova phenomena.
 

radiative shock,,supernovae,,scaling law