Abstract
We present our work to study the origin of the massive stars observed close to Sgr A*, the Galactic super‐massive black hole, and the dynamics of the massive stars' winds. We argue that the stars were formed in a ∼104 M⊙ accretion disc that existed around Sgr A* in the past. We find that the stellar dynamics constrain the total mass of the stellar population, requiring the mass function to be dominated by massive stars. We present a numerical study of star formation in a massive disc and show the influence of radiative cooling on the resulting mass function. We also present simulations of the accretion of stellar winds onto Sgr A*. We first discuss the strong influence of the stellar dynamics on the accretion onto the central black hole. From realistic simulations of Sgr A* accretion we find that slow winds shock and rapidly cool, forming cold gas clumps and filaments that coexist with the hot X‐ray emitting gas. The accretion rate is highly variable on time‐scales of tens to hundreds of years. Such varia...
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
