Supermassive star formation via episodic accretion: protostellar disc instability and radiative feedback efficiency

Understand

The formation of SMSs is a potential pathway to seed SMBHs in the early universe.

• A critical issue for forming SMSs is stellar UV feedback, which may limit the stellar mass growth via accretion.
• In this paper we study the evolution of an accreting SMS and its UV emissivity under conditions of realistic variable accretion from a self-gravitating circumstellar disc.
• First we conduct a 2D hydrodynamical simulation to follow the long-term protostellar accretion until the stellar mass exceeds $10^4~M_\odot$.