منابع مشابه
Analytic Study of Mass Segregation around a Massive Black Hole
We analyze the distribution of stars of arbitrary mass function g(m) around a massive black hole (MBH). Unless g is strongly dominated by light stars, the steady-state distribution function approaches a power-law in specific energy x ≡ −E/mσ2 < xmax with index p = m/4M0, where E is the energy, σ the typical velocity dispersion of unbound stars, and M0 the mass averaged over mgx p max. For light...
متن کاملStrong Mass Segregation around a Massive Black Hole
We show that the mass-segregation solution for the steady state distribution of stars around a massive black hole (MBH) has two branches: the known weak segregation solution (Bahcall & Wolf 1977), and a newly discovered strong segregation solution, presented here. The nature of the solution depends on the heavy-tolight stellar mass ratio MH/ML and on the unbound population number ratio NH/NL, t...
متن کاملViolent Relaxation Around a Massive Black Hole
I present galaxy models resulting from violent relaxation in the presence of a pre-existing black hole. The models are computed by maximizing the entropy of the stellar dynamical system. I show that their properties are very similar to those of adiabatic growth models for a suitable choice of parameters. This suggests that observations of nuclear light profiles and kinematics alone may not be s...
متن کاملThe Efficiency of Resonant Relaxation around a Massive Black Hole
Resonant relaxation (RR) is a rapid relaxation process that operates in the nearly-Keplerian potential near a massive black hole (MBH). RR dominates the dynamics of compact remnants that inspiral into a MBH and emit gravitational waves (extreme mass ratio inspiral events, EMRIs). RR can either increase the EMRI rate, or strongly suppress it, depending on its still poorly-determined efficiency. ...
متن کاملOscillation phenomena in the disk around the massive black hole
We report the detection of radio QPOs with structure changes using the Very Long Baseline Array (VLBA) at 43 GHz. We found conspicuous patterned changes of the structure with P = 16.8, 22.2, 31.4,&56.4 min, roughly in a 3 : 4 : 6 : 10 ratio. The first two periods show a rotating one-arm structure, while the P = 31.4 min shows a rotating 3-arm structure, as if viewed edge-on. At the central 50μa...
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ژورنال
عنوان ژورنال: The Astrophysical Journal
سال: 2009
ISSN: 0004-637X,1538-4357
DOI: 10.1088/0004-637x/698/1/l64