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| Format: | Preprint |
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2026
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| Online Access: | https://arxiv.org/abs/2603.15791 |
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| _version_ | 1866912969270493184 |
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| author | Ouyed, Rachid |
| author_facet | Ouyed, Rachid |
| contents | We show that delayed (weeks-months) energy injection into expanding Type Ic supernova (SN) ejecta can reproduce the luminosity and spectral evolution of hydrogen-poor superluminous SNe (SLSNe-I). Late-time reheating sets the radiation temperature and density needed for the W-shaped OII absorption near peak, explaining its disappearance as the ejecta cools without extra excitation mechanisms. In our model, the neutron star (NS) undergoes a core phase transition to deconfined quark matter at time t_QN, triggering rapid magnetic field amplification and forming a hybrid star (HS; a QCD-magnetar). This Quark-Nova (QN) resets the central engine, weeks to months after the SN, by converting the NS rotational energy into renewed energy injection, producing two powering epochs separated by a delay determined by hadron-to-quark microphysics. The model reproduces photometric and spectroscopic evolution of SLSNe-I such as iPTF13ajg, SN2010gx, PTF09cnd, and PTF09atu. We predict a systematic offset between spectroscopic and photometric ages when pre-QN emission is below detection limits, and discuss observational signatures distinguishing QCD-magnetars from standard magnetars. Double-peaked SLSNe-I may probe the hadron-quark transition, constraining quark-matter parameters like deconfinement density and surface tension. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2603_15791 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | Late-Onset Energy Injection in Type Ic SNe and W-Shaped O II Absorption in SLSNe-I Ouyed, Rachid High Energy Astrophysical Phenomena Solar and Stellar Astrophysics We show that delayed (weeks-months) energy injection into expanding Type Ic supernova (SN) ejecta can reproduce the luminosity and spectral evolution of hydrogen-poor superluminous SNe (SLSNe-I). Late-time reheating sets the radiation temperature and density needed for the W-shaped OII absorption near peak, explaining its disappearance as the ejecta cools without extra excitation mechanisms. In our model, the neutron star (NS) undergoes a core phase transition to deconfined quark matter at time t_QN, triggering rapid magnetic field amplification and forming a hybrid star (HS; a QCD-magnetar). This Quark-Nova (QN) resets the central engine, weeks to months after the SN, by converting the NS rotational energy into renewed energy injection, producing two powering epochs separated by a delay determined by hadron-to-quark microphysics. The model reproduces photometric and spectroscopic evolution of SLSNe-I such as iPTF13ajg, SN2010gx, PTF09cnd, and PTF09atu. We predict a systematic offset between spectroscopic and photometric ages when pre-QN emission is below detection limits, and discuss observational signatures distinguishing QCD-magnetars from standard magnetars. Double-peaked SLSNe-I may probe the hadron-quark transition, constraining quark-matter parameters like deconfinement density and surface tension. |
| title | Late-Onset Energy Injection in Type Ic SNe and W-Shaped O II Absorption in SLSNe-I |
| topic | High Energy Astrophysical Phenomena Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2603.15791 |