Speaker: Kuria Watanabe<\/p>\n\n\n\n
Abstract:<\/p>\n\n\n\n
Chemical properties of young galaxies are important to understand the chemical evolution in galaxy formation. We investigate the origin of abundance ratios in JWST star-forming galaxies (z ~ 4-10) by comparing chemical evolution models.
The high N\/O ratio in GN-z11, CEERS_01019, and GLASS_150008 observed with JWST cannot be explained by typical chemical evolution models including AGB stars. We focus on the three candidates of rich nitrogen, the Wolf-Rayet stars (WR), supermassive stars (SMS), and tidal disruption events (TDE). We develop the chemical evolution models of three candidates. Although the Ar\/O values of the high N\/O galaxies are not obtained, we find that the Ar\/O values are the key to distinguishing between the three models. The three models can show the high N\/O values as much as the N\/O values in GN-z11, CEERS_01019, and GLASS_150008. Because the time scale of high N\/O is very short due to the CCSNe, the massive stars (>25 Msun) should directly collapse into black holes.<\/p>\n","protected":false},"excerpt":{"rendered":"