S22A0050

P Cygni is the nearest Luminous Blue Variable (LBV) star. Flash mass-loss events, which are called as outbursts, drive the LBV evolutionary process, and circumstellar nebulae around LBV stars provide essential clues for the outbursts. Near-infrared [Fe II] emission is a powerful tool for investigating shocks produced by the outbursts. In our recent paper, we have discovered a compact but intrinsically extended [Fe II] emission region, with FWHM of ∼3^′′. Its origin is unclear but the plausible scenario is that the young and small outburst occurred 50 years before has made the shock shell. If proved, it will give us the mass-loss history, which strongly constrains the LBV evolutional process. In order to investigate the detailed structure of this newly-found region, we propose an AO-IFU observation by Gemini/NIFS. First, we will calculate the mass loss rate precisely with the spatially-resolved observation. Secondly, we directly compare the shell geometry with the simulation to test the LBV outburst mechanism currently considered. P Cygni is the best target for this study; its nebula is expanded with no/little interaction with the external structures, unlike η Carinae.

This document was translated from L^AT_EX by H^EV^EA.