DYNAMICAL CONSTRAINTS ON THE ORIGIN OF THE YOUNG B-STARS IN THE GALACTIC CENTER

Journal Article · Tue Aug 10 04:00:00 EDT 2010 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/719/1/220· OSTI ID:21455024

Perets, Hagai B ^[1]; Gualandris, Alessia ^[2]

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1. Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138 (United States)
2. Max-Planck-Institut fuer Astrophysik, Karl-Schwarzschild-Str. 1, D-85741 Garching (Germany)

Regular star formation is thought to be inhibited close to the massive black hole (MBH) in the Galactic center. Nevertheless, tens of young main-sequence B-stars have been observed in an isotropic distribution close to it. These stars are observed to have an apparently continuous distribution from very close to the MBH (<0.01 pc) and up to at least {approx}0.5 pc, suggesting a common origin. Various models have been suggested for the formation of the B-stars closest to the MBH (<0.05 pc; the S-stars), typically involving the migration of these stars from their original birthplace to their currently observed position. Here, we explore the orbital phase space distribution of the B-stars throughout the central parsec expected from the various suggested models for the origin of the B-stars. We find that most of these models have difficulties in explaining, by themselves, both the population of the S-stars (<0.05 pc) and the population of the young B-stars further away (up to 0.5 pc). Most models grossly overpredict the number of B-stars up to 0.5 pc, given the observed number of S-stars. Such models include the intermediate-mass black hole assisted cluster inspiral scenario, Kozai-like perturbations by two disks, spiral density waves migration in a gaseous disk, and some of the eccentric disk instability models. We focus on one of the other models, the massive perturbers induced binary disruption, which is consistent with both the S-stars and the extended population of B-stars further away. For this model, we use analytical arguments and N-body simulations to provide further observational predictions. These could be compared with future observations to further support this model, constrain it, or refute it. These predictions include the radial distribution of the young B-stars, their eccentricity distribution, and its dependence on distance from the MBH (higher eccentricities at larger distances from the MBH), as well as less specific expectations regarding their mass function.

• OSTI ID: 21455024
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 1 Vol. 719; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
BLACK HOLES
GALAXIES
GALAXY NUCLEI
INSTABILITY
MATHEMATICAL SPACE
PERTURBATION THEORY
PHASE SPACE
SIMULATION
SPACE
STARS