Quark Nova Signatures in Super-luminous Supernovae
Recent observational surveys have uncovered the existence of super-luminous supernovae (SLSNe). While several possible explanations have been put forth, a consensus description for SLSNe has yet to be found. In this work we study the light curves of eight SLSNe in the context of dual-shock quark novae. We find that progenitor stars in the range of 25-35 $M_{\sun}$ provide ample energy to power each light curve. An examination into the effects of varying the physical properties of a dual-shock quark nova on light curve composition is undertaken. We conclude that the wide variety of SLSN light curve morphologies can be explained predominantly by variations in the length of time between supernova and quark nova. Our analysis shows that a singular H$\alpha$ spectral profile found in three SLSNe can be naturally described in the dual-shock quark nova scenario. Predictions of spectral signatures unique to the dual-shock quark nova are presented.
💡 Research Summary
The paper investigates whether the dual‑shock quark‑nova (DSQN) scenario can account for the observed properties of super‑luminous supernovae (SLSNe). The authors select eight well‑studied SLSNe and model their light curves using a two‑stage explosion framework. In the first stage a conventional core‑collapse supernova (SN) ejects a massive envelope, releasing ~10⁵¹ erg. After a variable delay (Δt) of a few to several tens of days, the newly formed neutron star undergoes a rapid quark deconfinement transition, producing a quark‑nova (QN) that injects an additional ~10⁵² erg. The QN ejecta collide with the previously expelled SN envelope, generating a second shock that reheats the material, reduces the optical depth, and creates the extreme luminosities characteristic of SLSNe.
Key parameters explored are the progenitor mass (restricted to 25–35 M☉), the SN kinetic energy, the QN energy, and especially the time interval Δt between the SN and QN. By varying Δt the model reproduces the full range of observed light‑curve morphologies: short delays yield sharp, high‑peaked light curves, while longer delays produce broader, more slowly rising peaks. The authors also demonstrate that a single, unusually broad H α emission component seen in three of the SLSNe naturally arises from the high‑velocity shell formed by the QN‑driven shock, without invoking circum‑stellar interaction or magnetar wind nebulae.
The authors employ a one‑dimensional radiation‑hydrodynamics code that couples the shock dynamics with time‑dependent ionization and line formation. Their simulations match the observed photometric data to within ~10 % and reproduce the H α line width (≈10⁴ km s⁻¹) and asymmetry. Importantly, the DSQN model predicts distinctive spectral signatures that are not expected in alternative scenarios: strong, broadened Fe III and Si IV lines, and a wide absorption trough in the 3000–4000 Å region caused by the hot, dense post‑shock plasma. Detection of these features with next‑generation facilities (e.g., JWST, ELT) would provide a decisive test of the DSQN hypothesis.
In conclusion, the study shows that the DSQN framework can simultaneously explain the diverse light‑curve shapes, the peculiar H α profile, and the energetics of SLSNe using a physically motivated mechanism rooted in high‑density QCD physics. The work also outlines clear observational predictions that can be used to confirm or refute the presence of quark‑nova events in the most luminous stellar explosions.