Possible Structure and Origin of the Dark Mass Concentration in the Galactic Center.

Details Possible Structure and Origin of the Dark Mass Concentration in the Galactic Center. Possible Structure and Origin of the Dark Mass Concentration in the Galactic Center.

Apr 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aps..apr..n905o&link_type=abstract

American Physical Society, APS/AAPT Joint April Meeting, April 18-21, 1998 Columbus, Ohio, abstract #N9.05

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An extended, nearly isothermal cluster of normal stars with a core radius of ~0.5 pc in the Galactic center contains dark matter (DM) inferred from dynamical considerations. I assume the DM in the central 1 pc of the Galaxy consists of two major components: (i) an extended (although highly concentrated) cluster of compact stellar remnants (CSRs), such as neutron stars and stellar black holes (*BHs), plus (ii) a point central mass, a massive black hole (MBH). The MBH could have formed either prior to the Galaxy formation (Option I) or as a result of the dynamical evolution of the stellar nucleus (Option II). For Option II, I explore whether the central part of the multi-mass system of CSRs is in the state of a bounced core collapse. The bounce could occur as a result of heating produced by *BH binaries formed by the three-body process (H.M. Lee, 1995, MNRAS 272, 605). Then the DM cluster experiences the slow expansion accompanied by core oscillations, during which the central point mass -- a MBH -- could be formed. The inferred density of stars wihin the central ~ 0.01 pc of the Galaxy is consistent with what would be expected if the core were in the post-bounced state of gravo-thermal oscillations. However, if further, higher resolution data on velocity dispersion confirm its increase ∝ r-1/2 towards smaller radii, it would be strong evidence in favor of a single central MBH, possibly of primordial origin.

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