Thermonuclear Supernovae: Prospecting in the Age of Time-Domain and Multi-wavelength Astronomy

Abstract

We show how new and upcoming advances in the age of timedomain and multi-wavelength astronomy will open up a new venue to probe the diversity of SN Ia. We discuss this in the context of the ELT (ESO), as well as space based instrument such as James Webb Space Telescope (JWST). As examples we demonstrate how the power of very early observations, within hours to days after the explosion, and very late-time observations, such as light curves and mid-infraread spectra beyond 3 years, can be used to probe the link to progenitors and explosion scenarios. We identify the electron-capture cross sections of Cr, M n, and N i/Co as one of the limiting factors we will face in the future.

The core normal Type Ia supernova 2019np – an overall spherical explosion with an aspherical surface layer and an aspherical 56Ni core

“…It emerges from the fitting when introduced as an additional free parameter not included in the hydrodynamical model. Possible physical causes may include a short-lived interaction between the SN ejecta with a low-mass accretion disc (Gerardy et al 2007 ) or a companion star (Marietta et al 2000 ), or surface burning as found in sub-M Ch explosions (Shen et al 2012 ) but see item (3), or the imprint of the burning of H/He-rich material originating from the surface (Hoeflich et al 2019 ). Interaction with a donor star seems less likely because it would affect not only the outermost layers.…”

“…1 ), corresponding to the very outer layers of ࣠ 4 × 10 −3 M ⊙ , making a sub-M Ch explosion an unlikely candidate even for the case of C/He mixtures (Shen & Moore 2014 ). Note that M Ch explosions may have a thin H/He-rich surface layer as a result of the accretion phase but at a significantly smaller mass, (1-5) × 10 −4 M ⊙ (Hoeflich et al 2019 ), an amount below our numerical resolution. Therefore, we neglect the H/He layer in our simulation.…”

Type Ia Supernova Progenitor Properties and their Host Galaxies

“…17 For example, to first order and as an upper limit, we may expect similar EC isotopes in HeD and DDT at 1.2 and 1.3 Me, respectively. However, the duration of compression by a detonation is shorter than the WD expansion timescale resulting in about one-half the shift in abundance with respect to from partial to NSE burning (log(ρ c )  −1), EC isotopes (log(ρ c ) ³ 8.5, 54 Fe, 57 Co, 58 Ni), and to increasingly neutron-rich isotopes from 55,56 Fe, 55 Mn to 48,52,54 Cr, 59,60 Fe (log(ρ c ) ³ 1.87), which is close to the accretion induced collapse (Höflich et al 1998b;Brachwitz et al 2000;Hoeflich et al 2019).…”

Type Ia supernovae in the age of JWST: Finding the ‘right’ questions and the path to answers

“…1). Geometry is sensitive to the companion star and the [7]. Middle: Temperature and turbulent velocity structure at the onset of thermonuclear runaway of the inner 100 km of a WD [8].…”

“…Figure1: Progenitor structure and multi-dimensional imprints. Upper left: Central WD density as a function of mass and the influence of element production[7]. Middle: Temperature and turbulent velocity structure at the onset of thermonuclear runaway of the inner 100 km of a WD[8].…”