In this episode, we explore the extraordinary discovery of SN 2024afyu, a nearby supernova located at redshift (z = 0.0085) (approx. 37.7 Mpc). Featuring an unusually slow 85-day rise to peak brightness and a peak magnitude of (M_r = -18.9 mag), this supernova challenges standard core-collapse models. We discuss how its massive synthesized Nickel and Sulfur components make SN 2024afyu one of the strongest candidates ever observed for a Pair-Instability Supernova (PISN)—a catastrophic thermonuclear explosion triggered by electron–positron pair creation in massive stellar cores.
Key Topics Covered
A Slow Cosmic Burn: Why SN 2024afyu's broad light curve and 85-day rise time set it apart from typical Type II and Type IIb supernovae.
Chemical Anomalies: The early emergence of forbidden calcium ([Ca II]) lines without typical oxygen emission, alongside unique optical and near-infrared sulfur emission features ([S I], [S II], and [S III]).
Evaluating the Explosion Engine: How the heavy yields of intermediate-mass elements rule out standard core-collapse mechanisms, magnetar spin-down, and black hole fallback accretion.
Comparing with Theoretical PISN Models: How spectral and photometric observations compare against low-redshift pair-instability models.
The Host Galaxy: Insights into 2MFGC 13744, a star-forming dwarf galaxy providing the low-metallicity environment expected for massive PISN progenitors.
### Article Reference
Title: SN 2024afyu interpreted as a Pair Instability Supernova (arXiv preprint: SN 2024afyu: A Candidate Pair-Instability Supernova with Peculiar Evolution)
Authors: P. J. Pessi, S. Barmentloo, Ł. Wyrzykowski, S. Schulze, J. Sollerman, A. Gangopadhyay, P. J. Mikołajczyk, S. Rose, K. Kotysz, C. Fremling, et al.
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