Star Formation Close to Sgr A* and Beyond the Nuclear Cluster

Abstract

Two modes of star formation are involved to explain the origin of young stars near Sgr A*. One is a disk-based mode, which explains the disk of stars orbiting Sgr A*. The other is the standard cloud-based mode observed in the Galactic disk. We discuss each of these modes of star formation and apply these ideas to the inner few parsecs of Sgr A*. In particular, we focus on the latter mode in more detail. We also discuss how the tidal force exerted by the nuclear cluster makes the Roche density approaching zero and contributes to the collapse of molecular clouds located tens of parsecs away from Sgr A*.

4 pages, 2 figures, International Astronomical Union Proceedings Series 324, editors: Andreja Gomboc and Carole Mundell

References in corpus (6)

• The Two Young Star Disks in the Central Parsec of the Galaxy: Properties, Dynamics and Formation
• On the Formation of Compact Stellar Disks Around Sgr A*
• Radio Continuum Observations of the Galactic Center: Photoevaporative Proplyd-like Objects near Sgr A*
• Galactic Center Mini-spiral by ALMA - Possible Origin of the Central Cluster
• Signatures of Young Star Formation Activity Within Two Parsecs of Sgr A*
• Stability of Gas Clouds in Galactic Nuclei: An Extended Virial Theorem