Speaker
Description
Supernova (SN) explosions are fundamental phenomena representing the final stages of stellar evolution, during which an enormous amount of energy is released over a short period of time. The radiation emitted during the explosion can interact with the circumstellar material (CSM), which can significantly affect the observed light curves (LCs) and spectra.
A classic example of this phenomenon is SN 1987A, a hydrogen-rich Type II SN. Interestingly, its spectroscopic properties resembled those of Type IIP SN, while its LC exhibited a different evolution. Objects similar to SN 1987A constitute a rare class of SNe, although the circumstances of their formation are still not fully understood. The hypothesis of this research is that the properties of peculiar SNe resembling SN 1987A but exhibiting stronger radiation–matter interaction – such as the shape of the LC, late-time rebrightening, or the appearance of characteristic emission lines – can be explained by substantial mass loss prior to the explosion and the presence of dense circumstellar material.
In recent years, several peculiar SNe similar to SN 1987A but exhibiting more pronounced radiation–matter interaction have been identified; SN 2026ejy is one such example. The physical properties of SN 2026ejy make it a suitable target for investigating the physical characteristics indicative of circumstellar interaction with sufficient accuracy using the available instruments and data-processing methods. The aim of my research is to perform a consistent analysis of the observations of these objects, with particular focus on SN 2026ejy, complemented by the observations of the 80 cm telescope of the SZTE Baja Observatory, and to determine their physical parameters and perform a comparative analysis using photometric and spectroscopic methods. This investigation may contribute to a deeper understanding of the nature of SN 1987A-like SNe.