X-rays from cusps of compact remnants near galactic centres

Details X-rays from cusps of compact remnants near galactic centres X-rays from cusps of compact remnants near galactic centres

2006-11-10

arxiv.org/abs/astro-ph/0611345v1

Mon.Not.Roy.Astron.Soc.377:1647-1651,2007

Astronomy and Astrophysics

Astrophysics

submitted to MNRAS; 5 pages

Scientific paper

10.1111/j.1365-2966.2007.11725.x

Compact remnants -- stellar mass black holes and neutron stars formed in the inner few parsec of galactic centres are predicted to sink into the central parsec due to dynamical friction on low mass stars, forming a high concentration cusp (Morris 1993). Same physical region may also contain very high density molecular clouds and accretion discs that are needed to fuel SMBH activity. Here we estimate gas capture rates onto the cusp of stellar remnants, and the resulting X-ray luminosity, as a function of the accretion disc mass. At low disc masses, most compact objects are too dim to be observable, whereas in the high disc case most of them are accreting at their Eddington rates. We find that for low accretion disc masses, compact remnant cusps may be more luminous than the central SMBHs. This ``diffuse'' emission may be of importance for local moderately bright AGN, especially Low Luminosity AGN. We also briefly discuss how this expected emission can be used to put constraints on the black hole cusp near our Galactic Centre.

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