The $γ$-ray deposition histories of Calcium-rich supernovae

Amir Sharon; Doron Kushnir

doi:10.1093/mnras/stad1227

paper

The $γ$ -ray deposition histories of Calcium-rich supernovae

arXiv:2212.14290 · doi:10.1093/mnras/stad1227

Abstract

Calcium-rich supernovae (Ca-rich SNe) are faint, rapidly evolving transients whose progenitor system is yet to be determined. We derive the $γ$ -ray deposition histories of five Ca-rich SNe from the literature in order to place constraints on possible progenitor systems. We find that the $γ$ -ray escape time, $t_{0}$ , of the Ca-rich SNe sample is $\approx 35$ - $65 d$ , within the unoccupied region between Type Ia SNe and stripped envelope supernovae (SESNe). The $t_{0}$ - $M_{Ni56}$ distribution of these SNe, where $M_{Ni56}$ is the synthesised $^{56}$ Ni mass in the explosion, creates a continuum between the Type Ia and SESNe $t_{0}$ - $M_{Ni56}$ distribution, hinting at a possible connection between all the events. By comparing our results to models from the literature, we were able to determine that helium shell detonation models and core-collapse models of ultra-stripped stars are unlikely to explain Ca-rich SNe, since the gamma-ray escape time in these models is smaller than the observed values. Models that agree with the observed $t_{0}$ - $M_{Ni56}$ distribution are explosions of low mass, $M \approx 0.75$ - $0.8 M_{⊙}$ , white dwarfs and core-collapse models of stripped stars with an ejecta mass of $M \approx 1$ - $3 M_{⊙}$ .

arXiv comment12 pages, submitted to MNRAS

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The γ-ray deposition histories of Calcium-rich supernovae

Abstract

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Cited by in corpus (1)

The $γ$ -ray deposition histories of Calcium-rich supernovae