Speaker: Gábor Gyula, KISS (ATOMKI)
Title: What we can learn about supernovae with particle accelerators
Place: Wigner FK RMI III. ép. Tanácsterem
Date: 17 March 2023, 14:00
The exponential technical development that took place in the first two decades of the 20th century opened up new horizons in astronomy. Nowadays, we can detect the gravitational waves (and electromagnetic radiation) emitted after the merger of neutron stars and study the composition of the very old stars located at the edge of our Galaxy [Cov21]. If we associate the information obtained through these observations with precise nuclear physics data, we can obtain information on the characteristics of astronomical objects, as well as the nucleosynthesis processes taking place in them.
The technical development did not leave the instruments of experimental nuclear physics untouched either. In the most advanced accelerator centres that produce radioactive beams, in some cases, nuclei created during explosive nucleosynthesis processes can be produced, their properties and decay methods can be examined, and thus we can gain insight into nucleosynthesis processes [Kis22].
However, we don't need to travel to, for example, Japan if we want to study such processes experimentally! The combination of research infrastructures available in Hungary, i.e. at the Atomki and Wigner research institutes, offers a unique opportunity to study the reactions playing key role in the synthesis of neutron-rich nuclei found between strontium and silver. In my presentation, I would like to present three measurements carried out using different techniques (partly in progress), through which it is possible to obtain information about the characteristics of the material ejected during the supernova explosion and the nucleosynthesis process taking place [Kis21, Sze22, Psa22].
[Cov21] J. J. Cowan et al., Rev. Mod. Phys. 93 (2021) 015002
[Kis21] G. G. Kiss et al., Astrophysical J. 908 (2021) 202
[Kis22] G. G. Kiss et al., Astrophysical J. 936 (2022) 107
[Psa22] A. Psaltis et al., Astrophysical J. 935 (2022) 27
[Sze22] T. N. Szegedi et al., Phys. Rev. C 100 (2021) 035804