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| Format: | Preprint |
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2025
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| Online Access: | https://arxiv.org/abs/2512.16554 |
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| _version_ | 1866917154175057920 |
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| author | Shiran, Kobi Soker, Noam |
| author_facet | Shiran, Kobi Soker, Noam |
| contents | 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 shell is motivated by the morphologies of several CCSN remnants whose structures have been attributed to multiple pairs of jets in the framework of the jittering jets explosion mechanism (JJEM). The deduced multiple-shell ejecta of SN 2024ggi in this study, and of SN 2023ixf in an earlier study, as well as studies of the polarization of SN 2024ggi, are better compatible with the JJEM than with the neutrino-driven mechanism. Our study supports the growing evidence that the JJEM is the primary explosion mechanism of CCSNe. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2512_16554 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Double shell structure in supernova 2024ggi Shiran, Kobi Soker, Noam High Energy Astrophysical Phenomena 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 shell is motivated by the morphologies of several CCSN remnants whose structures have been attributed to multiple pairs of jets in the framework of the jittering jets explosion mechanism (JJEM). The deduced multiple-shell ejecta of SN 2024ggi in this study, and of SN 2023ixf in an earlier study, as well as studies of the polarization of SN 2024ggi, are better compatible with the JJEM than with the neutrino-driven mechanism. Our study supports the growing evidence that the JJEM is the primary explosion mechanism of CCSNe. |
| title | Double shell structure in supernova 2024ggi |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2512.16554 |