2024/03/20 by Paul C. Duffell, Abigail Polin, Duffell, Paul C. +3
Physics and Astronomy · #Astrophysics and Cosmic Phenomena #FOS: Physical sciences #Gamma-ray bursts and supernovae #High Energy Astrophysical Phenomena (astro-ph.HE) #Neutrino Physics Research
paper · pdf · doi:10.48550/arxiv.2403.13641
openalex publication_date 2024/03/20 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We demonstrate in a proof-of-concept numerical hydrodynamics calculation that the narrow radial filamentary structures seen in Pa 30 could be generated through highly efficient cooling (e.g. via line emission) in the ejecta. Efficient cooling in the ejecta causes a drop of pressure support in Rayleigh-Taylor fingers, leading them to be compressed, and suppressing the growth of Kelvin-Helmholtz instability. Following this result, we make three predictions that could determine whether this is the mechanism responsible for shaping Pa 30: First, we predict very strong emission lines, strong enough to cool a significant fraction of the shock energy in an expansion time. Secondly, we predict that the forward shock should be highly corrugated on small scales, with the shock front closely following the structure of the filaments. Third, we predict that these filaments should be nearly ballistic, with velocities around 90% of the free-expansion velocity (v ≈ 0.9 ~r/t). These predictions should be falsifiable in follow-up observations of this remnant.