Modeling Supernova 2023ixf: Lightcurve Degeneracies and Morphological Differences
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arXiv
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| Autori principali: | , |
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| Natura: | Preprint |
| Pubblicazione: |
2025
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| _version_ | 1866916693578612736 |
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| author | Forde, Shannon Goldberg, Jared A. |
| author_facet | Forde, Shannon Goldberg, Jared A. |
| contents | Supernova 2023ixf is a type IIP supernova that was observed in May 2023 in the spiral galaxy Messier 101. This was the closest supernova observed of the decade, making this an exciting discovery. Combining the observed brightness and duration with theoretical scaling relations, we model the lightcurve of this supernova in order to reveal the properties of the progenitor star at the time of explosion, including its mass, radius, and explosion energy. We simulate these explosions using the stellar evolution and radiation-hydrodynamics codes MESA+STELLA. We find that SN2023ixf is not easily explained with "normal" stellar evolution, and only models with a small mass of H-rich ejecta can fit the lightcurve. We also find that the late time properties of the lightcurve are better fit by a higher initial-mass star with substantial mass loss during its lifetime, as compared to models with lower initial mass and less mass loss. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2504_12421 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Modeling Supernova 2023ixf: Lightcurve Degeneracies and Morphological Differences Forde, Shannon Goldberg, Jared A. Solar and Stellar Astrophysics Astrophysics of Galaxies High Energy Astrophysical Phenomena Supernova 2023ixf is a type IIP supernova that was observed in May 2023 in the spiral galaxy Messier 101. This was the closest supernova observed of the decade, making this an exciting discovery. Combining the observed brightness and duration with theoretical scaling relations, we model the lightcurve of this supernova in order to reveal the properties of the progenitor star at the time of explosion, including its mass, radius, and explosion energy. We simulate these explosions using the stellar evolution and radiation-hydrodynamics codes MESA+STELLA. We find that SN2023ixf is not easily explained with "normal" stellar evolution, and only models with a small mass of H-rich ejecta can fit the lightcurve. We also find that the late time properties of the lightcurve are better fit by a higher initial-mass star with substantial mass loss during its lifetime, as compared to models with lower initial mass and less mass loss. |
| title | Modeling Supernova 2023ixf: Lightcurve Degeneracies and Morphological Differences |
| topic | Solar and Stellar Astrophysics Astrophysics of Galaxies High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2504.12421 |