Galactic Dynamics: Second Edition

By J. Binney, S. Tremaine. 2008

3,864 citations recorded by the source corpus.

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

Yule-Simpson’s paradox in Galactic Archaeology (2019, background): “…shown before in observations, although it could be argued would result from the scatter plots shown in Figures 5 and 7 by Ramı́rez et al. (2012) and should correspond to bins of common stellar mass, shown in several works (e.g., Nissen & Schuster 2012; Ramı́rez et al. 2012; Bensby & Lind 2018).”
Rates of compact object coalescences (2021, background): “In the classical version of dynamical formation in a dense stellar environment the black holes, being heavier than other cluster objects, sink toward the centre of the cluster through mass segregation (Spitzer, 1969; Binney and Tremaine, 2008).”
Integral field spectroscopy with SINFONI of VVDS galaxies I. Galaxy dynamics and mass assembly at 1.2 < z < 1.6 (2009, background): “Binney & Tremaine (2008) suggest that C = 2.25 is an average value of known galactic mass distribution models.”
The old Nuclear Star Cluster in the Milky Way (2014, methodology): “From the tensor virial theorem (Binney & Tremaine 2008) we know that for 2I-models υ2Φ > υ 2 R in order to produce the flattening.”
Rapid and Bright Stellar-mass Binary Black Hole Mergers in Active Galactic Nuclei (2016, positive): “Using M• = M0(σ/σ0)k according to the M• −σ relation, and taking σ0 = 200km/s, M0 = 1.3×108M and k = 4 (Binney & Tremaine 2008; Gültekin et al. 2009), we obtain Rinf = GM• σ2 = GM0 σ20 ( M• M0 )1−(2/k) = 1.2M1/26 pc , (6) where M6 ≡M•/106M .”
The SLUGGS Survey: kinematics for over 2500 globular clusters in 12 early-type galaxies (2012, background): “The galaxy anisotropy has classically been measured through the parameter β that gives the relative ratio of the tangential to the radial velocity dispersion for a given dynamical tracer (Binney & Tremaine 2008).”
TDCOSMO IV: Hierarchical time-delay cosmography -- joint inference of the Hubble constant and galaxy density profiles (2020, positive): “…spherically symmetric system, with the only distinction between radial,σ2r , and tangential,σ 2 t , dispersions, the Jeans equation results in (e.g., Binney & Tremaine 2008) ∂(ρ∗σ2r (r)) ∂r + 2βani(r)ρ∗(r)σ2r (r) r = −ρ∗(r) ∂Φ(r) ∂r , (10) with the stellar anisotropy parameterized as βani(r) ≡ 1…”
THE MEGAMASER COSMOLOGY PROJECT. III. ACCURATE MASSES OF SEVEN SUPERMASSIVE BLACK HOLES IN ACTIVE GALAXIES WITH CIRCUMNUCLEAR MEGAMASER DISKS (2010, background): “…the half-mass relaxation timescale; Binney & Tremaine 2008) is considered to be the upper limit of the lifetime of any bound stellar system whereas the collision timescale is the characteristic timescale that a star suffers a physical collision (i.e. an inelastic encounter; Binney & Tremaine 2008).”
Constraining the Milky Way assembly history with Galactic Archaeology (2016, background): “This spiral lifetime is most likely a low limit because of the quick disc heating taking place in these simulations, due to the lack of gas infall, which, if present, would rejuvenate the spiral structure (Binney & Tremaine, 2008).”
Axion dark matter, solitons and the cusp–core problem (2015, background): “On length scales larger than the soliton radius the usual thermodynamic arguments relating to dust (Binney & Tremaine 2008) will apply, leading to an NFW-like profile (on large scales this equivalence between the Schrödinger picture and dust thermodynamics can be derived using the Wigner…”
Cosmological simulations with self-interacting dark matter – II. Halo shapes versus observations (2012, methodology): “The third way we will quantify halo shapes observationally is in terms of similar spheroids (see, e.g., Section 2.5 of Binney & Tremaine 2008).”
KINEMATICS OF THE STELLAR HALO AND THE MASS DISTRIBUTION OF THE MILKY WAY USING BLUE HORIZONTAL BRANCH STARS (2012, background): “The tidal effects of LMC and SMC on 2 The disk model withb = 0 is also otherwise known as Toomre’s model or Kuzmin disk (Toomre 1963; Binney & Tremaine 2008) 0 20 40 60 80 100 120 140 160 180 r (kpc) 0 50 100 150 200 250 300 350 v c ir c ( km s− 1 ) X08 W99S09 G10 W10 S11 D12b Figure 11.”
Characterizing the gravitational instability in cooling accretion discs (2008, background): “…azimuthal wavelength,|kR| ≫ m, with R the cylindrical radius) we have D(ω, k,m) = (ω − mΩ)2 − c2sk2 + 2πGΣ|k| − κ2 = 0, (1) whereΩ(R) is the angular speed, andκ(R) is the epicyclic frequency,cs(R) is the sound speed andΣ(R) is the surface density of the umperturbed disc (Binney & Tremaine 2008).”
MINOR MERGERS AND THE SIZE EVOLUTION OF ELLIPTICAL GALAXIES (2009, methodology): “According to the virial theorem (Binney & Tremaine 2008) the total energy of the system is Ei = Ki + Wi = −Ki = 1 2 Wi = − 1 2 Mi〈v 2 i 〉 = − 1 2 GM2i rg,i .”
Kinematics in Young Star Clusters and Associations with Gaia DR2 (2018, methodology): “On the other hand, for the Plummer sphere and the lowered isothermal sphere models (also known as King models), velocity dispersions decrease monotonically with radius (Binney & Tremaine 2008).”
Rotational support of giant clumps in high-z disc galaxies (2011, methodology): “The Jeans equation inside the clump then reads (e.g. Binney & Tremaine 2008, eq.”
WIDE-FIELD PRECISION KINEMATICS OF THE M87 GLOBULAR CLUSTER SYSTEM (2011, positive): “4.215 of Binney & Tremaine 2008).”
Formation of Galaxy Clusters (2012, methodology): “For a collisionless system of particles, such as CDM, the conditi of equilibrium is given by the Jeans equation (e.g., Binney & Tremaine 2008).”
Greatly Enhanced Merger Rates of Compact-object Binaries in Non-spherical Nuclear Star Clusters (2017, neutral): “The evaporation time can be estimated as (Binney & Tremaine 2008): τevap= (m1 +m2)σ 16 √ πGainm2ν ln Λ = 3× 108 ( ln Λ 2 )−1 × ( m1 +m2 20M⊙ )( MBH 4× 106M⊙ )−1 ( σ 100km s−1 ) × ( ain 10AU )−1 ( mν 5× 105M⊙ pc−3 )−1 yr.”