Double shell structure in supernova 2024ggi
Kobi Shiran, Noam Soker (Technion, Israel)

TL;DR
This paper presents a simple two-shell model for supernova ejecta that explains the evolution of the photospheric radius in SN 2024ggi, supporting the jittering jets explosion mechanism over neutrino-driven models.
Contribution
The study introduces a toy model with a spherical and an elongated shell to reproduce supernova photospheric evolution, favoring the jittering jets explosion mechanism.
Findings
The two-shell model reproduces the observed photospheric radius evolution.
The model explains the transition from concave to convex Rph(t).
Results support the jittering jets explosion mechanism as the primary CCSN driver.
Abstract
We built a simple toy model of a core-collapse supernova (CCSN) ejecta composed of two shells, an outer low-mass spherical shell and an inner elongated massive shell, and show that it can reproduce the evolution of the photospheric radius of SN 2024ggi, Rph(t). During the first week, the larger spherical shell, the S-shell, forms the photosphere. As the shell expands and becomes increasingly transparent, the photosphere moves inward along the mass coordinate, although it grows in size. When the photosphere reaches the long axis of the elongated inner shell, the E-shell begins to contribute to the photosphere, ultimately comprising the entire photosphere. The simple toy model explains the transition of Rph(t) from being concave (decreasing slope) to convex (increasing slope). A single-shell model predicts only concave behavior. The structure of a spherical shell with an inner elongated…
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Taxonomy
TopicsGamma-ray bursts and supernovae · Neutrino Physics Research · Astrophysics and Cosmic Phenomena
