Abstract
The supermassive black hole at the Galactic center is surrounded by a parsec-scale star disk, with about a hundred massive young stars that move in approximately circular Keplerian orbits. Another group of roughly 20 young stars ("S-stars") follow eccentric, randomly oriented orbits well inside the disk stars. A model is proposed to explain the S-stars. Accordingly, the stars formed originally in the parsec-scale disk through gravitational fragmentation of gas. The newly formed S-stars then migrated inward via the gravitational torques exerted by a Lin-Shu-type spiral density wave on the stars at an inner Lindblad resonance.
| Original language | English |
|---|---|
| Pages (from-to) | L1-L4 |
| Journal | Astrophysical Journal |
| Volume | 702 |
| Issue number | 1 PART 2 |
| DOIs | |
| State | Published - 1 Jan 2009 |
Keywords
- Black hole physics
- Galaxy: center
- Stellar dynamics
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science