arXiv subjects

Charles J. Aouad

Publications and source records attributed to Charles J. Aouad.

3 recordsLinked to original sources

arXiv2026

Abundance Stratification in Type Ia Supernovae -- VIII. The 03fg-like SN\,2012dn: a double-degenerate merger interpretation

A detailed study using abundance tomography of SN 2012dn, a peculiar Type Ia supernova, is presented. Despite exhibiting a normal peak luminosity, it retains early-phase super-Chandrasekhar (03fg-like) characteristics: weak Fe III, narrow intermediate-mass element (IME), persistent carbon, and the absence of high-velocity Ca II features. Its nebular spectrum is unusually faint due to grey dimming beginning $\sim$60 days after maximum and shows [O I] emission, rare in SNe Ia. While a Chandrasekhar-mass density profile reproduces the photospheric phase, it fails at late times. The [O I] emission requires additional low-velocity mass, implying a total ejecta mass of $1.66$ $M_\odot$, including $0.33$ $M_\odot$ of oxygen (with $0.1$ $M_\odot$ in the core). The $^{56}$Ni mass is estimated to be $0.45$--$0.49$ $M_\odot$, a range set by uncertainties in the grey-extinction correction applied at the nebular phase, and is insufficient on its own to account for the peak luminosity. Stable iron is confined to intermediate layers and absent from both the core and outer ejecta, the latter indicating sub-solar progenitor metallicity. Silicon and sulfur span the full ejecta, while carbon extends down to $v \sim 6000$ ${\rm km,s^{-1}}$. These properties favour a double-degenerate CO--CO white dwarf merger scenario. The remaining luminosity deficit may be explained by additional energy input from a weak interaction with a low-mass, carbon-rich circumstellar shell.

astro-ph.HE↗

arXiv2024

Abundance stratification in type Ia supernovae -- VII. The peculiar, C-rich iPTF16abc: highlighting diversity among luminous events

Observations of Type Ia supernovae (SNe\,Ia) reveal diversity, even within assumed subcategories. Here, the composition of the peculiar iPTF16abc (SN\,2016bln) is derived by modeling a time series of optical spectra. iPTF16abc's early spectra combine traits of SNe 1999aa and 1991T known for weak \SiII\ $λ$ 6355 and prominent \FeIII\ features. However, it differs with weak early \FeIII\ lines, and persistent \CII\ lines post-peak. It also exhibits a weak \CaII\ H\&K feature aligning it with SN\,1991T, an observation supported by their bolometric light curves. The early attenuation of \FeIII\ results from abundance effect. The weakening of the \SiII\ $λ$ 6355 line, stems from silicon depletion in the outer shells, a characteristic shared by both SNe 1999aa and 1991T, indicating a common explosion mechanism that terminates nuclear burning at around 12000 \kms\, unseen in normal events. Beneath a thin layer of intermediate mass elements (IMEs) with a total mass of 0.18 \Msun, extends a \Nifs\ rich shell totaling 0.76 \Msun\ and generating a bolometric luminosity as high as ${L_{\mathrm{peak}}}=1.60 \pm 0.1 \times$ $10^{43}$ ergs s$^{-1}$. Inner layers, typical of SNe\,Ia, hold neutron-rich elements, (\Feff\ and \Nife), totaling 0.20 M${\odot}$. Stable iron, exceeding solar abundance, and carbon, coexist in the outermost layers, challenging existing explosion models. The presence of carbon down to $v\approx$ 9000\,\kms, totalling $\sim$ 0.01 \Msun\, unprecedented in this class, links iPTF16abc to SN\,2003fg-like events. The retention of 91T-like traits in iPTF16abc underscores its importance in understanding the diversity of SNe\,Ia.

astro-ph.HE↗

arXiv2022

Abundance stratification in type Ia supernovae -- VI: the peculiar slow decliner SN\,1999aa

The abundance distribution in the ejecta of the peculiar slowly declining Type Ia supernova (SN\,Ia) SN\,1999aa is obtained by modelling a time series of optical spectra. Similar to SN\,1991T, SN\,1999aa was characterised by early-time spectra dominated by \FeIII\ features and a weak \SiII\,6355\,Å line, but it exhibited a high-velocity \CaII\,H\&K line and morphed into a spectroscopically normal SN\,Ia earlier. Three explosion models are investigated, yielding comparable fits. The innermost layers are dominated by $\sim 0.3$\,\Msun\ of neutron-rich stable Fe-group elements, mostly stable iron. Above that central region lies a \Nifs-dominated shell, extending to $v \approx 11,000$ -- $12,000$\,\kms, with mass $\sim 0.65$\,\Msun. These inner layers are therefore similar to those of normal SNe\,Ia. However, the outer layers exhibit composition peculiarities similar to those of SN\,1991T: the intermediate-mass elements shell is very thin, containing only $\sim 0.2$\,\Msun, and is sharply separated from an outer oxygen-dominated shell, which includes $\sim 0.22$\,\Msun. These results imply that burning suddenly stopped in SN\,1999aa. This is a feature SN\,1999aa shares with SN\,1991T, and explain the peculiarities of both SNe, which are quite similar in nature apart from the different luminosities. The spectroscopic path from normal to SN\,1991T-like SNe\,Ia cannot be explained solely by a temperature sequence. It also involves composition layering differences, suggesting variations in the progenitor density structure or in the explosion parameters.

astro-ph.HE↗