Dynamics and Evolution of Galactic Nuclei

By D. Merritt. 2013

400 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/5452f4927069c11eb0dec55f57c3e8ffd61111f1

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Citations in the corpus

The old Nuclear Star Cluster in the Milky Way (2014, methodology): “The relaxation time of the NSC within 1 pc is tr ∼ 10(10) yr (Alexander 2005; Merritt 2013), indicating that the NSC is not fully relaxed and is likely to be evolving. One would expect from theoretical models that, if relaxed, the stellar density near the SMBH should be steeply-rising and form a Bah”
BLACK HOLE TRIPLE DYNAMICS: A BREAKDOWN OF THE ORBIT AVERAGE APPROXIMATION AND IMPLICATIONS FOR GRAVITATIONAL WAVE DETECTIONS (2013, background): “The result is a set of first-order differential equations that describe the long-term (secular) evolution of the remaining orbital elements due to the perturbing forces (Merritt 2013).”
Greatly Enhanced Merger Rates of Compact-object Binaries in Non-spherical Nuclear Star Clusters (2017, methodology): “The value of Γco depends on the assumed IMF and on the star formation history of the NC. Table 1 in Löckmann et al. (2010) gives the composition of an evolved stellar population for different star formation histories and IMFs; we use this table to compute Γco.”
Rapid and Bright Stellar-mass Binary Black Hole Mergers in Active Galactic Nuclei (2016, background): “Note that the cluster around M• & 107M may not be relaxed within a Hubble time at least for a single-mass-component (Merritt 2013).”
On the rate of black hole binary mergers in galactic nuclei due to dynamical hardening (2017, methodology): “…to calculate the rate of single-binary encounters, we adopt the density profile given by Equations 1 and 4 in Merritt (2010) for the velocity-dispersionsupported component with a central density of 106 M⊙ pc −3, a half-mass radius of rh = 2.5 pc (Merritt 2013) and a mass-to-light ratio of 2.”
Surface brightness profile of the Milky Way’s nuclear star cluster (2014, methodology): “Deviation from sphericity have been addressed in the context of triaxial bulges, bars or stellar discs, on scales of 100 – 1000 pc, but also a number of theoretical studies have investigated non-spherical structures of the nucleus itself (Holley-Bockelmann et al. 2001, 2002; Berczik et al. 2006; Mer”
Stellar Dynamics and Stellar Phenomena Near a Massive Black Hole (2017, background): “This simple picture of binary separation is further complicated by the finite size of the stars, which for some initial parameters results in stellar collisions and occasional mergers instead of ejections Ginsburg & Loeb (2007); Antonini et al. (2010); Antonini, Lombardi & Merritt (2011).”
On the charge of the Galactic centre black hole (2018, neutral): “≈ 100 km s−1, we get (see e.g. Merritt 2013; Generozov et al. 2015), Rinf ' GM•/σ2?”
A bright year for tidal disruptions (2015, background): “5.267 of Merritt (2013), which describe exactly the relativistic, inclination-dependent change in BH spin following accretion of stellar matter; however, the simple Newtonian estimate of equation 8 However, the maximum spin that can be reached through constant prograde accretion depends on…”
Selection bias in dynamically measured supermassive black hole samples: its consequences and the quest for the most fundamental relation (2016, background): “…in this paper – but they are not supported by observations. c© 2016 RAS, MNRAS000, 1– 20 ics is expected to be dominated by the black hole (e.g., Merritt & Ferrarese 2001b), and not adequately resolving the sphere of influence could significantly bias black hole mass estimates (e.g., Merritt 2013).”
The astrophysics of nanohertz gravitational waves (2018, background): “1998), galactic velocity dispersion (Ferrarese & Merritt 2000; Gebhardt et al. 2000), and Sérsic index (Graham & Driver 2007), amongst other properties. This suggests that SMBHs co-evolve with their host galaxies. These relations have been critical throughout astronomy because of their ability to pr”
The Galaxy in Context: Structural, Kinematic, and Integrated Properties (2016, background): “2009); this might indicate that the NSC is not fully relaxed, consistent with the relaxation time estimated as ≈10 Gyr throughout the NSC (Merritt 2013).”