As part of a collaboration lead by Alexandra Kozyreva and Raphael Hirschi, I have contributed to the study of pair-instability supernovae (PISNe) models for high-mass stars at relatively high metallicity. According to our stellar evolution calculations, these models do not retain any hydrogen in the outer layers at the point of explosion. Using detailed radiative transfer calculations, we determined synthetic observables for pair-instability supernovae occurring in such stars and found that their light curves are relatively fast evolving. Thus, such events may be suitable candidates to explain some superluminous supernovae. Additionally, an important part of this study was the investigation associated with the light curve modelling. Here, we focussed mainly on the consequences of using different radiative transfer tools, relying on different opacity prescriptions and including the so-called nickel-bubble effect. Our results are summarized in a paper which has just been accepted for publication in MNRAS. A preprint may be found on the arXiv or on the early access system of MNRAS.

The most luminous thermonuclear supernovae (SNe) still constitute puzzles. Reconciling their intense luminosities with the standard theoretical interpretation for Type Ia SNe, according to which the light output is predominantly attributable to the decay of radioactive elements, would require very high nickel masses, implying ejecta masses beyond the Chandrasekhar mass - hence their other name, “Super-Chandrasekhar” explosions.

An important step in the development of the Monte Carlo Radiation Hydrodynamical approach MCRH has been completed. Having demonstrated the basic operation of this method and an application to Type Ia supernova ejecta in a first paper, we have now successfully used MCRH in the context of momentum-driven mass outflows from hot stars.

Together with Stefan Taubenberger and Emille Ishida, I’ve spent three nights at the Observatory of Padova University in Asiago. We used the telescope on Cima Ekar to classify and perform follow-up observations of a number of transient objects. Some of our findings are summarized in the Atels 1, 2 and 3.