Galactic Dynamics: Second Edition
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The CMZ is thought to originate as a result of gas dynamics within the Galactic bar.
“The CMZ is thought to originate as a result of the gas dynamics within the Galactic bar.”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Binney & Tremaine 2008
Stable orbits in the bar potential (x1 orbits) become intersecting when the orbital energy reaches a critical value.
“Stable orbits in the bar potential ( x 1 orbits) become intersecting when the orbital energy reaches a critical value (Binney & Tremaine 2008).”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Binney & Tremaine 2008
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Coevolution (Or Not) of Supermassive Black Holes and Host Galaxies
Kormendy, J., & Ho, L. C. (2013) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-082708-101811 · Cited by 4,198 · see citing works
Harko, T., Lobo, F. S. N., Nojiri, S., & Odintsov, S. D. (2011) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.84.024020 · Cited by 2,780 · see citing works
Local kinematics and the local standard of rest
Schönrich, R. A., Binney, J. J., & Dehnen, W. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.16253.x · Cited by 1,921 · see citing works
“The theoretical underpinning of this method is the asymmetric drift relation (see Binney & Tremaine 2008, eq.”
MethodSelf-citationUltralight scalars as cosmological dark matter
Hui, L., Ostriker, J. P., Tremaine, S. D., & Witten, E. (2017) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.95.043541 · Cited by 1,710 · see citing works
Self-citationgalpy: A python LIBRARY FOR GALACTIC DYNAMICS
Bovy, J. (2015) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/216/2/29 · Cited by 1,543 · see citing works
“…list thereof to be used. solar radius5 R0 for populations with different radial-velocity dispersions and investigate how they depend on the asymmetric drift, i.e., the offset between the mean rotational velocity of a kinematically warm population and the circular velocity (Binney & Tremaine 2008).”
BackgroundMethodResultInfluentialCoevolution (Or Not) of Supermassive Black Holes and Host GalaxiesPreprint
Kormendy, J., & Ho, L. C. (2013) · Cited by 1,437 · see citing works
UniverseMachine: The correlation between galaxy growth and dark matter halo assembly from z = 0−10
Behroozi, P., Wechsler, R. H., Hearin, A. P., & Conroy, C. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz1182 · Cited by 1,243 · see citing works
“In addition, harassment from other satellites is problematic because high velocities inside clusters mean that strong interactions are less likely to occur (Binney & Tremaine 2008).”
BackgroundThe Galactic Center massive black hole and nuclear star cluster
Genzel, R., Eisenhauer, F., & Gillessen, S. (2010) · Reviews of Modern Physics · doi:10.1103/revmodphys.82.3121 · Cited by 1,236 · see citing works
From dwarf spheroidals to cD galaxies: simulating the galaxy population in a ΛCDM cosmology
Guo, Q., White, S. D. M., Boylan-Kolchin, M., Lucia, G. D., Kauffmann, G., Lemson, G., Li, C., Springel, V., & Weinmann, S. M. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.18114.x · Cited by 1,205 · see citing works
“The structure and evolution of the two components is quite strongly coupled (e.g. Binney & Tremaine (2008) section 6.6), but our simple model nevertheless gives some indication of the extent to which misalignments might reflect changes with time in the orientation of accreted angular momentum.”
BackgroundInfluentialZwart, S. P., McMillan, S., & Gieles, M. (2010) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-081309-130834 · Cited by 926 · see citing works
“• Static Models are self-consistent potential–density pairs for specific choices of phasespace distribution functions (Plummer 1911, King 1966, Binney & Tremaine 2008).”
BackgroundTHE SINS SURVEY: SINFONI INTEGRAL FIELD SPECTROSCOPY OF z ∼ 2 STAR-FORMING GALAXIES
Schreiber, N. M. F., Genzel, R., Bouché, N., Cresci, G., Davies, R., Buschkamp, P., Shapiro, K. L., Tacconi, L. J., Hicks, E. K. S., Genel, S., et al. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/706/2/1364 · Cited by 1,115 · see citing works
FORMATION OF MASSIVE GALAXIES AT HIGH REDSHIFT: COLD STREAMS, CLUMPY DISKS, AND COMPACT SPHEROIDS
Dekel, A., Sari, R., & Ceverino, D. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/703/1/785 · Cited by 1,028 · see citing works
“In the solar neighborhood, (according to Binney & Tremaine 2008, §6.2.3), the gas fraction is ∼ 25%, the stars are much “hotter” than the gas, σg∗ ≃ 0.18, and the separate Q values are Qg ≃ 1.5 and Q∗ ≃ 2.7.”
BackgroundMethodInfluentialMINOR MERGERS AND THE SIZE EVOLUTION OF ELLIPTICAL GALAXIES
Naab, T., Johansson, P. H., & Ostriker, J. P. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/699/2/l178 · Cited by 984 · see citing works
“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 .”
MethodModified Newtonian Dynamics (MOND): Observational Phenomenology and Relativistic Extensions
Famaey, B., & McGaugh, S. S. (2012) · Living Reviews in Relativity · doi:10.12942/lrr-2012-10 · Cited by 911 · see citing works
“ct a relation a0 = V 4 f /(GM) for a point mass M. Since spiral galaxies are not point masses but rather flattened mass distributions that rotate faster than the equivalent spherical mass distribution [45], the empirical acceleration a is close to but not identical to a0 in MOND. The geometric correction is about 20% s…”
BackgroundMethodVERY HIGH GAS FRACTIONS AND EXTENDED GAS RESERVOIRS INz= 1.5 DISK GALAXIES
Daddi, E., Bournaud, F., Walter, F., Dannerbauer, H., Carilli, C. L., Dickinson, M., Elbaz, D., Morrison, G. E., Riechers, D. A., Onodera, M., et al. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/713/1/686 · Cited by 909 · see citing works
“We find the following best fitting relation to the actual mass insidere: M(r re) = 1.3× re× (vFWHM/2)2 G sin2 i ±12.5% (2) Thecorrection factorof 1.3 includes various effects: • the flattening of the baryonic mass distribution in a disk (Binney & Tremaine 2008).”
BackgroundInfluentialKravtsov, A. V., & Borgani, S. (2012) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-081811-125502 · Cited by 872 · see citing works
“For a collisionless system of particles, such as CDM, the conditi of equilibrium is given by the Jeans equation (e.g., Binney & Tremaine 2008).”
MethodCappellari, M., Scott, N., Alatalo, K., Blitz, L., Bois, M., Bournaud, F., Bureau, M., Crocker, A., Davies, R. L., Davis, T. A., et al. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt562 · Cited by 733 · see citing works
“(17) This formula is rigorously independent of anisotropy and only depends on the radial profiles of luminous and dark matter (Binney & Tremaine 2008, section 4.8.3).”
BackgroundMethodInfluentialTheoretical Challenges in Galaxy Formation
Naab, T., & Ostriker, J. (2016) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-081913-040019 · Cited by 441 · see citing works
“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〈v2i 〉 = − 1 2 GM2i rg,i .”
MethodCappellari, M., McDermid, R. M., Alatalo, K., Blitz, L., Bois, M., Bournaud, F., Bureau, M., Crocker, A., Davies, R. L., Davis, T. A., et al. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt644 · Cited by 695 · see citing works
Accurate masses for dispersion-supported galaxies
Wolf, J., Martinez, G. D., Bullock, J. S., Kaplinghat, M., Geha, M., Muñoz, R. R., Simon, J. D., & Avedo, F. F. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.16753.x · Cited by 691 · see citing works
A UNIVERSAL MASS PROFILE FOR DWARF SPHEROIDAL GALAXIES?
Walker, M. G., Mateo, M. L., Olszewski, E. W., Peñarrubia, J., Evans, N. W., & Gilmore, G. F. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/704/2/1274 · Cited by 673 · see citing works
THE SINS SURVEY OF z ∼ 2 GALAXY KINEMATICS: PROPERTIES OF THE GIANT STAR-FORMING CLUMPS
Genzel, R., Newman, S., Jones, T., et al. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/733/2/101 · Cited by 681 · see citing works
“…vc, epicyclic frequency κ (κ2 = 4 (vc/Rdisk)2 + Rdisk d(vc/Rdisk)2/dRdisk), gas surface density Σgas, and radius of the disk Rdisk via the relation (Binney & Tremaine 2008; Escala & Larson 2008; Elmegreen 2009; Dekel et al. 2009a) Qgas = σ0κ πGΣgas = ( σ0 vc ) ( a ( v2cRdisk/G ) πR2diskΣgas…”
Star Clusters Across Cosmic Time
Krumholz, M. R., McKee, C. F., & Bland‐Hawthorn, J. (2019) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-091918-104430 · Cited by 657 · see citing works
A METHOD FOR MEASURING (SLOPES OF) THE MASS PROFILES OF DWARF SPHEROIDAL GALAXIES
Walker, M. G., & Peñarrubia, J. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/742/1/20 · Cited by 683 · see citing works
“Stellar Kinematics with Two Numbers In principle the Collisionless Boltzmann Equation (CBE, Equation 4.6 of Binney & Tremaine 2008) relates the 6- dimensional phase-space distribution function,f (~r ,~v), of a tracer component to the underlying gravitational potential, thereby governing the joint…”
BackgroundInfluentialGenzel, R., Burkert, A., Bouché, N., Cresci, G., Schreiber, N. F. F., Shapley, A., Shapiro, K., Tacconi, L., Buschkamp, P., Cimatti, A., et al. (2008) · The Astrophysical Journal · doi:10.1086/591840 · Cited by 536 · see citing works
“In the approximation of a very large and very thin disk, this is given by hz=R ¼ 0:5 02=vdð Þ2; ð1aÞ where vd(R) is the rotation velocity at radius R (Binney & Tremaine 2008, eq.”
BackgroundMethodRapid and Bright Stellar-mass Binary Black Hole Mergers in Active Galactic Nuclei
Bartos, I., Kocsis, B., Haiman, Z., & Szabolcs Marka, C. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/835/2/165 · Cited by 586 · see citing works
“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 .”
InfluentialCompaction and quenching of high-z galaxies in cosmological simulations: blue and red nuggets
Zolotov, A., Dekel, A., Mandelker, N., et al. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv740 · Cited by 574 · see citing works
“For an isothermal sphere or for an exponential disk at the exponential radius,α ≃ 2 (Burkert et al. 2010; Binney & Tremaine 2008).”
BackgroundSimon, J. D. (2019) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-091918-104453 · Cited by 610 · see citing works
Dynamical Origin of Extrasolar Planet Eccentricity Distribution
Jurić, M., & Tremaine, S. D. (2008) · The Astrophysical Journal · doi:10.1086/590047 · Cited by 561 · see citing works
Self-citationCosmological simulations with self-interacting dark matter – II. Halo shapes versus observations
Peter, A. H. G., Rocha, M., Bullock, J. S., & Kaplinghat, M. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sts535 · Cited by 510 · see citing works
“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).”
BackgroundMethodInfluentialEvidence for two early accretion events that built the Milky Way stellar halo
Myeong, G. C., Vasiliev, E., Iorio, G., Evans, N. W., & Belokurov, V (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz1770 · Cited by 505 · see citing works
Structure and Kinematics of Early-Type Galaxies from Integral Field Spectroscopy
Cappellari, M. (2016) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-082214-122432 · Cited by 507 · see citing works
“To quantify this large amount of information, three anisotropy parameters were defined (Cappellari et al. 2007; Binney & Tremaine 2008, equation 4.265) βz ≡ 1− Πzz ΠRR , γ ≡ 1− Πφφ ΠRR , δ ≡ 1− Πzz Πxx , (7) where (R, z, φ) are the standard cylindrical coordinates, z coincides with the symmetry…”
BackgroundMethodInfluentialA dynamically young and perturbed Milky Way disk
Antoja, T., Helmi, A., Romero-Gómez, M., Katz, D., Babusiaux, C., Drimmel, R., Evans, D. W., Figueras, F., Poggio, E., Reylé, C., et al. (2018) · Nature · doi:10.1038/s41586-018-0510-7 · Cited by 498 · see citing works
Carollo, D., Beers, T. C., Chiba, M., Norris, J. E., Freeman, K. C., Lee, Y. S., Ivezić, Ž., Rockosi, C. M., & Yanny, B. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/712/1/692 · Cited by 479 · see citing works
“This form of f (e) is expected for a well-mixed steady-state system of test particles for which the distribution function is a function of the energy only, moving in the potential of a strongly centrally concentrated density distribution (see Binney & Tremaine, 2008, p. 387).”
Longair, M. S. (2011) · Cambridge University Press eBooks · doi:10.1017/cbo9780511778346 · Cited by 492 · see citing works
Read, J. I. (2014) · Journal of Physics G: Nuclear and Particle Physics · doi:10.1088/0954-3899/41/6/063101 · Cited by 489 · see citing works
Cool outflows in galaxies and their implications
Veilleux, S., Maiolino, R., Bolatto, A., & Aalto, S. (2020) · The Astronomy and Astrophysics Review · doi:10.1007/s00159-019-0121-9 · Cited by 289 · see citing works
“For a singular isothermal sphere, where the mass M( r) diverges at large r but the circular velocity vcirc is a constant, v2esc(r) = 2 v 2 circ ln(rhalo/r), so it slowly diverges for large rhalo/r (Binney and Tremaine 2008).”
BackgroundModified Newtonian Dynamics (MOND): Observational Phenomenology and Relativistic ExtensionsPreprint
Famaey, B., & McGaugh, S. (2012) · Cited by 454 · see citing works
The minimum-mass extrasolar nebula: in situ formation of close-in super-Earths
Chiang, E., & Laughlin, G. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt424 · Cited by 457 · see citing works
“(8) The Toomre stability parameter (e.g., Binney & Tremaine 2008) for our gas disk is Qgas = cgasΩ πGσgas = 15F −1disk ( a 0.2 AU )0.1 , (9) large enough compared to unity that the MMEN is gravitationally stable.”
InfluentialThe Evolution of the Star-Forming Interstellar Medium Across Cosmic Time
Tacconi, L. J., Genzel, R., & Sternberg, A. (2020) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-082812-141034 · Cited by 467 · see citing works
Chemodynamical evolution of the Milky Way disk
Minchev, I., Chiappini, C., & Martig, M. (2013) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201220189 · Cited by 454 · see citing works
“1, where we have corrected for asymmetric drift as described in, e.g., Binney and Tremaine (2008).”
MethodA million binaries from Gaia eDR3: sample selection and validation of Gaia parallax uncertainties
El-Badry, K., Rix, H., & Heintz, T. M. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab323 · Cited by 456 · see citing works
McDermid, R. M., Alatalo, K., Blitz, L., Bournaud, F., Bureau, M., Cappellari, M., Crocker, A., Davies, R. L., Davis, T. A., de Zeeuw, P. T., et al. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv105 · Cited by 443 · see citing works
“Our study also uses σ e: the velocity dispersion integrated within Re, which is empirically close to the true second velocity moment 〈v2los〉∞ that appears in the scalar virial theorem (Binney & Tremaine 2008), and is directly proportional to mass.”
MethodThe Local Dark Matter DensityPreprint
Read, J. I. (2016) · Cited by 439 · see citing works
Merger rate of primordial black-hole binaries
Ali-Haïmoud, Y., Kovetz, E. D., & Kamionkowski, M. (2017) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.96.123523 · Cited by 431 · see citing works
“The evaporation time is approximately [71]”
Forming Planetesimals in Solar and Extrasolar Nebulae
Chiang, E., & Youdin, A. N. (2010) · Annual Review of Earth and Planetary Sciences · doi:10.1146/annurev-earth-040809-152513 · Cited by 446 · see citing works
“In z, the particle’s equation of motion reads z̈ = −ż/ts − Ω(2)Kz (9) where the last term accounts for stellar gravity, for z ≪ r.”
InfluentialLau, E. T., Kravtsov, A. V., & Nagai, D. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/705/2/1129 · Cited by 430 · see citing works
Ferreira, E. G. M. (2021) · The Astronomy and Astrophysics Review · doi:10.1007/s00159-021-00135-6 · Cited by 443 · see citing works
NOMINAL VALUES FOR SELECTED SOLAR AND PLANETARY QUANTITIES: IAU 2015 RESOLUTION B3 * †
Prša, A., Harmanec, P., Torres, G., et al. (2016) · The Astronomical Journal · doi:10.3847/0004-6256/152/2/41 · Cited by 423 · see citing works
“Along with it, IAU 2015 Resolution B2 adopted the definition of the parsec to be exactly 648,000/π au (Binney & Tremaine 2008; see also Cox 2000).”
MethodThe ATLAS3D project - IV. The molecular gas content of early-type galaxies★
Young, L. M., Bureau, M., Davis, T. A., Combes, F., McDermid, R. M., Alatalo, K., Blitz, L., Bois, M., Bournaud, F., Cappellari, M., et al. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2011.18561.x · Cited by 419 · see citing works
“For a cluster such as Virgo, with several hundreds to thousands of galaxies, the relaxation time is at least 10 crossing times (Binney & Tremaine 2008) and the crossing times are of the order of a Gyr.”
BackgroundTHE MILKY WAY'S CIRCULAR-VELOCITY CURVE BETWEEN 4 AND 14 kpc FROM APOGEE DATA
Bovy, J., Allende Prieto, C., Beers, T. C., Bizyaev, D., da Costa, L. N., Cunha, K., Ebelke, G. L., Eisenstein, D. J., Frinchaboy, P. M., García Pérez, A. E., et al. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/759/2/131 · Cited by 413 · see citing works
“The asymmetric drift in the plane of the Galaxy of a population of stars is given by (e.g., Binney & Tremaine 2008) Vc(R)Va(R) σ2R(R) = 1 2 [ X2 − 1− ∂ ln ( ν∗σ 2 R ) ∂ lnR ] , (4) assuming that the radial–vertical velocity moment σRZ = 0 in the Galactic plane, for symmetry reasons.”
MethodStreams, Substructures, and the Early History of the Milky Way
Helmi, A. (2020) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-032620-021917 · Cited by 407 · see citing works
The Circular Velocity Curve of the Milky Way from 5 to 25 kpc
Eilers, A.-C., Hogg, D. W., Rix, H.-W., & Ness, M. K. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/aaf648 · Cited by 404 · see citing works
Formation and Evolution of Compact-object Binaries in AGN Disks
Tagawa, H., Haiman, Z., & Kocsis, B. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab9b8c · Cited by 393 · see citing works
“For the formation rate of binaries, we extend the rough derivation of Equation (7.111) in Binney & Tremaine (2008) to account for the limitations of a disk geometry and the destructive effect of the SMBH.”
BackgroundMethodInfluentialEvidence from the H3 Survey That the Stellar Halo Is Entirely Comprised of Substructure
Naidu, R. P., Conroy, C., Bonaca, A., Johnson, B. D., 丁, Y.-S. 源. T., Caldwell, N., Zaritsky, D., & Cargile, P. A. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/abaef4 · Cited by 399 · see citing works
“In the third panel, we depict a summary of actions in the form of (Jz–JR)/Jtot versus Jf/Jtot following Binney & Tremaine (2008) and Vasiliev (2019).”
MethodA NEW MECHANISM FOR RADIAL MIGRATION IN GALACTIC DISKS: SPIRAL-BAR RESONANCE OVERLAP
Minchev, I., & Famaey, B. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/722/1/112 · Cited by 385 · see citing works
“as shown in Binney and Tremaine (2008). The parameter α is related to the pitch angle of the spirals, p, by α = m cot(p).”
BackgroundMethodInfluentialPortail, M., Gerhard, O., Wegg, C., & Ness, M. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw2819 · Cited by 378 · see citing works
“Beyond corotation, the surface density becomes larger along the minor axis than along the major axis, as one would expect based on the linear perturbation of near circular orbit (Dehnen 2000; Binney & Tremaine 2008).”
BackgroundDYNAMICS OF SOLIDS IN THE MIDPLANE OF PROTOPLANETARY DISKS: IMPLICATIONS FOR PLANETESIMAL FORMATION
Bai, X., & Stone, J. M. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/722/2/1437 · Cited by 376 · see citing works
Birrer (2020) · doi:10.1051/0004-6361/202038861 · Cited by 396 · see citing works
Secular evolution in disk galaxies
Sellwood, J. A. (2014) · Reviews of Modern Physics · doi:10.1103/revmodphys.86.1 · Cited by 374 · see citing works
Hui, L. (2021) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-120920-010024 · Cited by 391 · see citing works
Kinematics in Young Star Clusters and Associations with Gaia DR2
Kuhn, M. A., Hillenbrand, L. A., Sills, A., Feigelson, E. D., & Getman, K. V. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/aaef8c · Cited by 354 · see citing works
“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).”
BackgroundMethodInfluentialGala: A Python package for galactic dynamics
Price-Whelan, A. M. (2017) · The Journal of Open Source Software · doi:10.21105/joss.00388 · Cited by 351 · see citing works
Formation of Galaxy ClustersPreprint
Kravtsov, A. V., & Borgani, S. (2012) · Cited by 345 · see citing works
ON THE LOCAL DARK MATTER DENSITY
Bovy, J., & Tremaine, S. D. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/756/1/89 · Cited by 353 · see citing works
“Equation (1) is typically used to estimate the asymmetric drift (Binney & Tremaine 2008): since V 2c = R∂Φ/∂R we find V 2c − V̄ 2 = σ2V − σ 2 U [ 1 + ∂ ln (νσ2U) ∂ lnR + 1 ν R σ2U ∂ (νσ2UW ) ∂Z ] .”
Self-citationPerryman, M. A. C. (2011) · Cambridge University Press eBooks · doi:10.1017/9781108304160 · Cited by 343 · see citing works
MODELING THE METALLICITY DISTRIBUTION OF GLOBULAR CLUSTERS
Muratov, A. L., & Gnedin, O. Y. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/718/2/1266 · Cited by 338 · see citing works
“These numbers are consistent with the observed amount of the disk and bulge stars and the atomic and molecular gas in the Galaxy (from Binney & Tremaine 2008).”
ResultEXTRACTING PLANET MASS AND ECCENTRICITY FROM TTV DATA
Lithwick, Y., Xie, J., & Wu, Y. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/761/2/122 · Cited by 336 · see citing works
“Instead, here we model our results by assuming that the free eccentricities of all planets are randomly drawn from a Rayleigh distribution (Binney & Tremaine 2008) with random phases, i.e., that the real and imaginary parts of the complex free eccentricities (zfree ≡ ex + iey) are drawn from…”
MethodThe evolution of the star-forming interstellar medium across cosmic time
Tacconi, L., Genzel, R., & Sternberg, A. (2020) · MPG.PuRe (Max Planck Society) · Cited by 326 · see citing works
GALAXIA: A CODE TO GENERATE A SYNTHETIC SURVEY OF THE MILKY WAY
Sharma, S., Bland‐Hawthorn, J., Johnston, K. V., & Binney, J. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/730/1/3 · Cited by 322 · see citing works
“…coordinates,vcirc(R) the circular velocity as a function of cylindrical radiusR andvad the asymmetric drift, which is given by the Stromberg’s relation (equation 4.228 in Binney & Tremaine 2008) vad(τ, R)= σ2R 2vc × ( d ln ρ d lnR + d lnσ2φ d lnR + 1− σ2φ σ2R + 1− σ 2 z…”
InfluentialSelf-citationOn the local dark matter densityPreprint
Bovy, J., & Tremaine, S. D. (2016) · Cited by 346 · see citing works
Self-citationDark matter cores all the way down
Read, J. I., Agertz, O., & Collins, M. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw713 · Cited by 317 · see citing works
Disruption of dark matter substructure: fact or fiction?
van den Bosch, F. C., Ogiya, G., Hahn, O., & Burkert, A. M. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx2956 · Cited by 312 · see citing works
“(2) (e.g., Spitzer 1987; Binney & Tremaine 2008).”
BackgroundInfluentialThe distribution of dark matter in galaxies
Salucci, P. (2019) · The Astronomy and Astrophysics Review · doi:10.1007/s00159-018-0113-1 · Cited by 307 · see citing works
THE SINS SURVEY: MODELING THE DYNAMICS OFz∼ 2 GALAXIES AND THE HIGH-zTULLY-FISHER RELATION
Cresci, G., Hicks, E. K. S., Genzel, R., et al. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/697/1/115 · Cited by 309 · see citing works
“This z-velocity dispersion σ01 is estimated in one of two ways: 1. using an approximation appropriate for large thin disks, in which it depends on the scale height and mass surface density (Binney & Tremaine 2008, eq.”
BackgroundGALACTOSEISMOLOGY: DISCOVERY OF VERTICAL WAVES IN THE GALACTIC DISK
Widrow, L. M., Gardner, S. V., Yanny, B., Dodelson, S., & Chen, H.-Y. (2012) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/750/2/l41 · Cited by 303 · see citing works
“The distribution function, density, and potential for the equilibrium solution are f0(z, vz) = ρ0 (2πσ 2)1/2 exp (−Ez/σ 2), (2) Ψ0(z) = 2σ 2 ln ( cosh ( z 2zd )) , ρ0(z) = ρ0sech2 ( z 2zd ) , (3) where ρ0 = σ 2/8πGz2d ((Spitzer 1942), see, also Binney & Tremaine (2008), problem 4.21).”
BackgroundInfluentialToy models for galaxy formation versus simulations
Dekel, A., Zolotov, A., Tweed, D., Cacciato, M., Ceverino, D., & Primack, J. R. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt1338 · Cited by 304 · see citing works
“The deceleration due to dynamical friction is approximated by the Chandrasekhar formula (Binney & Tremaine 2008, sec.”
MethodThe Circular Velocity Curve of the Milky Way from 5 to 25 kpc
Eilers, A., Hogg, D., Rix, H., & Ness, M. (2019) · MPG.PuRe (Max Planck Society) · Cited by 303 · see citing works
Unveiling the Universe with emerging cosmological probes
Moresco, M., Amati, L., Amendola, L., Birrer, S., Blakeslee, J. P., Cantiello, M., Cimatti, A., Darling, J., Valle, M. D., Fishbach, M., et al. (2022) · Living Reviews in Relativity · doi:10.1007/s41114-022-00040-z · Cited by 312 · see citing works
Courteau, S., Cappellari, M., de Jong, R. S., Dutton, A. A., Emsellem, É., Hoekstra, H., Koopmans, L. V. E., Mamon, G. A., Maraston, C., Treu, T., et al. (2014) · Reviews of Modern Physics · doi:10.1103/revmodphys.86.47 · Cited by 293 · see citing works
“59 If we rewrite the stationary CBE in cylindrical coordinates (R, z, φ) and assume axial symmetry and steady state, we obtain two non-trivial Jeans equations (Jeans 1922; Binney & Tremaine 2008, Eq.”
BackgroundMethodInfluentialStrongly baryon-dominated disk galaxies at the peak of galaxy formation ten billion years ago
Genzel, R., Schreiber, N. M. F., Übler, H., Lang, P., Naab, T., Bender, R., Tacconi, L. J., Wisnioski, E., Wuyts, S., Tal Alexander, A., et al. (2017) · Nature · doi:10.1038/nature21685 · Cited by 290 · see citing works
Footprints of the Sagittarius dwarf galaxy in the Gaia data set
Laporte, C. F. P., Minchev, I., Johnston, K. V., & Gómez, F. A. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz583 · Cited by 286 · see citing works
High-redshift clumpy discs and bulges in cosmological simulations
Ceverino, D., Dekel, A., & Bournaud, F. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.16433.x · Cited by 287 · see citing works
“According to the standard Toomre instability analysis (Toomre 1964; Binney & Tremaine 2008, chapter 6), a rotating disc becomes unstable to axi-symmetric modes once the local gravity overcomes both differential rotation and pressure due to turbulence or thermal motions.”
MethodA COMPLETE SPECTROSCOPIC SURVEY OF THE MILKY WAY SATELLITE SEGUE 1: THE DARKEST GALAXY
Simon, J. D., Geha, M., Minor, Q. E., Martinez, G. D., Kirby, E. N., Bullock, J. S., Kaplinghat, M., Strigari, L. E., Willman, B., Choi, P. I., et al. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/733/1/46 · Cited by 286 · see citing works
“Even if we assume (without any physical basis) that the mass distribution is arbitrarily truncated at the half-light radius, the instantaneous Jacobi radius (e.g., Binney & Tremaine 2008, Equation 8.91) for Segue 1 would be ∼ 250 pc.”
BackgroundInfluentialMackereth, J. T., Schiavon, R. P., Pfeffer, J., Hayes, C. R., Bovy, J., Anguiano, B., Prieto, C. A., Hasselquist, S., Holtzman, J., Johnson, J. A., et al. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty2955 · Cited by 285 · see citing works
Thin, thick and dark discs in ΛCDM
Read, J. I., Lake, G., Agertz, O., & Debattista, V. P. (2008) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2008.13643.x · Cited by 281 · see citing works
“The dotted blue line on this plot shows the expected orbit for LMC-10◦-abig assuming a static background potential and Chandrasekhar dynamical friction (Binney & Tremaine 2008).”
BackgroundShi, J.-M., Krolik, J. H., Lubow, S. H., & Hawley, J. F. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/749/2/118 · Cited by 311 · see citing works
“On the other hand, gravitational torques due to non-axisymmetric fluctuations in the stellar density might create stresses strong enough to overcome the reduction in gaseous disk mass. (Binney & Tremaine 2008).”
BackgroundThe observed spiral structure of the Milky Way
Hou, L. G., & Han, J. L. (2014) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201424039 · Cited by 282 · see citing works
“Most grand-design spiral galaxies approximate two-fold rotational symmetry (e.g, Knapen et al. 1992; Rozas et al. 1998; Binney & Tremaine 2008).”
BackgroundKinematics and history of the solar neighbourhood revisited
Aumer, M., & Binney, J. J. (2009) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.15053.x · Cited by 282 · see citing works
Self-citationFormation and Evolution of Compact-object Binaries in AGN Disks
Tagawa, H., Haiman, Z., & Kocsis, B. (2020) · Repository of the Academy's Library (Library of the Hungarian Academy of Sciences) · Cited by 276 · see citing works
Fan, J., Andrey Katz, A., Randall, L., & Matthew Reece, B. (2013) · Physics of the Dark Universe · doi:10.1016/j.dark.2013.07.001 · Cited by 282 · see citing works
“We also assume that the disk scale length Rd is comparable to that for baryons, around 3 kpc [46].”
MethodANGULAR MOMENTUM AND GALAXY FORMATION REVISITED
Romanowsky, A. J., & Fall, S. M. (2012) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/203/2/17 · Cited by 273 · see citing works
“The standard lore is that spiral bulges and low-luminosity ellipticals are near oblate-isotropic, with typical (v/σ)∗ ∼ 0.9 (Kormendy & Illingworth 1982; Davies et al. 1983; Binney & Merrifield 1998; Binney & Tremaine 2008).”
BackgroundInfluentialvan der Marel, R. P., & Kallivayalil, N. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/781/2/121 · Cited by 299 · see citing works
“Measurements of galaxy rotation curves form the foundation of much of our understanding of galaxy formation, structure, and dynamics (e.g., Binney & Merrifield 1998; Binney & Tremaine 2008; Mo, van den Bosch, & White 2010).”
BackgroundAxion dark matter, solitons and the cusp–core problem
Marsh, D. J. E., & Pop, A.-R. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv1050 · Cited by 267 · see citing works
“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…”
BackgroundRam pressure stripping in high-density environments
Boselli, A., Fossati, M., & Sun, M. (2021) · The Astronomy and Astrophysics Review · doi:10.1007/s00159-022-00140-3 · Cited by 111 · see citing works
Actions for axisymmetric potentials
Binney, J. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.21757.x · Cited by 266 · see citing works
Self-citationA lower bound on the mass of dark matter particles
Boyarsky, A. M., Oleg Ruchayskiy, C., & Iakubovskyi, D. (2009) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2009/03/005 · Cited by 264 · see citing works
A supermassive black hole in an ultra-compact dwarf galaxy
Seth, A. C., van den Bosch, R. C. E., Mieske, S., et al. (2014) · Nature · doi:10.1038/nature13762 · Cited by 265 · see citing works
Kuo, C. Y., Braatz, J. A., Condon, J. J., et al. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/727/1/20 · Cited by 264 · see citing works
“…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).”
BackgroundInfluentialDawes Review 4: Spiral Structures in Disc Galaxies
Dobbs, C. L., & Baba, J. (2014) · Publications of the Astronomical Society of Australia · doi:10.1017/pasa.2014.31 · Cited by 267 · see citing works
“…the linearised equations of motion, and Poisson’s equation for a stellar disc, and established solutions which have the Fourier decomposition (Shu 1992; Binney & Tremaine 2008): ψ(R, φ, t) = Re[A(R)ei(ωt−mφ)], (1) where p = ω/m and p is the angular velocity of the perturbation, or pattern speed.”
BackgroundInfluential
- Authors
- Binney, J., & Tremaine, S.
- Venue
- Princeton University Press eBooks
- Publisher
- Princeton University Press
- Published
- 2008-12-31
- OpenAlex
- W1631788275
- Cited by
- 4,375
- References
- 0
- Citations by year
- 2026: 192 · 2025: 224 · 2024: 246 · 2023: 261 · 2022: 233 · 2021: 298 · 2020: 349 · 2019: 372 · 2018: 313 · 2017: 201 · 2016: 252 · 2015: 233 · 2014: 240 · 2013: 233 · 2012: 202
- FWCI
- 138.34
- Type
- book
- Language
- en
- Open access
- closed
- Locations
- Princeton University Press eBooks (publishedVersion)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysical Phenomena and Observations
- Keywords
- galaxy dynamics, galaxies, stellar dynamics, galaxy structure, galaxy evolution
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