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Branch of astrophysics
Stellar dynamics is the branch of astrophysics which describes in a statistical way the collective motions of stars subject to their mutual gravity. The
Stellar_dynamics
Subfield of astronomy
theoretical astrophysicists include Solar System formation and evolution; stellar dynamics and evolution; galaxy formation and evolution; magnetohydrodynamics;
Astrophysics
Indian-American physicist (1910–1995)
contributing to the contemporary understanding of stellar structure, white dwarfs, stellar dynamics, stochastic process, radiative transfer, the quantum
Subrahmanyan_Chandrasekhar
Coming together of two stars
A stellar collision is the coming together of two stars caused by stellar dynamics within a star cluster, or by the orbital decay of a binary star due
Stellar_collision
Subfield of astronomy
dynamics of electrically conducting fluids such as plasmas in astrophysical contexts. Magnetogravity wave – Coupled Alfvén-gravity waves in stellar interiors
Outline_of_astrophysics
Study of the movement of stars
black hole at the Galactic Center. Stellar kinematics is related to but distinct from the subject of stellar dynamics, which involves the theoretical study
Stellar_kinematics
Soviet astrophysicist
of the pioneers of Russian and world stellar dynamics. T. A. Agekian found two evolutionary sequences of stellar systems: nearly spherical and strongly
Tateos_Agekian
Study of forces and their effect on motion
Langevin dynamics, a mathematical model for stochastic dynamics Orbital dynamics, the study of the motion of rockets and spacecraft Stellar dynamics, a description
Dynamics_(mechanics)
explain the relaxation over time of the dynamics of N-body gravitating systems such as star clusters and galaxies. Stellar systems observed in the Universe –
Gurzadyan–Savvidy_relaxation
Dutch astrophysicist (born 1952)
for Advanced Studies, he conceived NEMO, a software environment for stellar dynamics, together with Josh Barnes and Peter Teuben. Hut introduced the concept
Piet_Hut
Alteration of orbits of celestial bodies through gravity
scattering clarifies several astrophysical problems, from stellar-cluster evolution to galaxy-core dynamics. In dense regions such as star clusters, scattering
Gravitational_scattering
Maximum mass of a stable white dwarf star
Chandrasekhar chose to move on, leaving the study of stellar structure to focus on stellar dynamics. In 1983 in recognition for his work, Chandrasekhar
Chandrasekhar_limit
cluster Stellar collision Stellar core Stellar coronae Stellar density Stellar disk Stellar distance Stellar drift Stellar dynamics Stellar engine Stellar envelope
List_of_stellar_properties
Classification of stars based on spectral properties
In astronomy, stellar classification is the classification of stars based on their spectral characteristics. Electromagnetic radiation from the star is
Stellar_classification
In astrophysics, the Chandrasekhar virial equations are a hierarchy of moment equations of the Euler equations, developed by the Indian American astrophysicist
Chandrasekhar virial equations
Chandrasekhar_virial_equations
Scottish applied mathematician and astronomer
at the University of Edinburgh. His main research interests are in stellar dynamics. Heggie has conducted pioneering theoretical research on the topic
Douglas_C._Heggie
British astronomer (born 1950)
Oxford University Press, 2025. Stellar Dynamics for Physicists, by James Binney, Kindle Direct Publishing, 2026. Stellar Dynamics: Problems with Solutions by
James_Binney
American astronomer and mathematician
Jack Gilbert Hills (born 15 May 1943) is a theorist of stellar dynamics. He worked on the Oort cloud; the inner part of it, the Hills cloud, was named
Jack_G._Hills
Galaxy in the constellation Sculptor
most complicated structures awaiting its explanation on the basis of stellar dynamics." The Third Reference Catalogue of Bright Galaxies (RC3) measured a
Cartwheel_Galaxy
Branch of astronomy involving positioning and movements of celestial bodies
celestial mechanics, stellar dynamics and galactic astronomy. In observational astronomy, astrometric techniques help identify stellar objects by their unique
Astrometry
Subrahmanyan, and Subrahmanyan Chandrasekhar. An introduction to the study of stellar structure. Vol. 2. Courier Corporation, 1958. Chandrasekhar, S., and Gordon
Emden–Chandrasekhar_equation
Gravitational loss of momentum and energy by bodies moving through surrounding matter
mass black holes.[citation needed] Globular clusters orbiting through the stellar field of a galaxy experience dynamic friction. This drag force causes the
Dynamical_friction
Phenomenon in astrophysics
Astrophysics: Gas dynamics. University Science Books. p. 147. ISBN 978-0-935702-65-1. Murray, C.D., and S.F. Dermott 1999, Solar System Dynamics (Cambridge:
Lindblad_resonance
Lucey, J. R.; Edge, A. C. (2017). "Stellar dynamics in the strong-lensing central galaxy of Abell 1201: A low stellar mass-to-light ratio a large central
List of most massive black holes
List_of_most_massive_black_holes
Jakob Karl Ernst Halm (1866 – 1944) was a pioneer of stellar dynamics and the first person to suggest the existence of a mass–luminosity relation for stars
Jakob_Karl_Ernst_Halm
Topics referred to by the same term
Australian open source electricity system model NEMO (Stellar Dynamics Toolbox), a toolbox for stellar dynamics modeling Neutrino Ettore Majorana Observatory
Nemo
Relation between density and radius for a white dwarf
Subrahmanyan, and Subrahmanyan Chandrasekhar. An introduction to the study of stellar structure. Vol. 2. Chapter 11 Courier Corporation, 1958. Davis, Harold
Chandrasekhar's white dwarf equation
Chandrasekhar's_white_dwarf_equation
Press, 1969. Binney, James; Tremaine, Scott (30 October 2011). Galactic Dynamics (Second ed.). Princeton University Press. pp. 59–60. ISBN 978-1400828722
Chandrasekhar potential energy tensor
Chandrasekhar_potential_energy_tensor
Cluster of stars around a supermassive black hole
A hypercompact stellar system (HCSS) is a dense cluster of stars around a supermassive black hole that has been ejected from the center of its host galaxy
Hypercompact_stellar_system
Equation of stability for a star
Hydrodynamic and hydromagnetic stability. Courier Corporation, 2013. Binney, James, and Scott Tremaine. Galactic dynamics. Princeton university press, 2011.
Chandrasekhar's variational principle
Chandrasekhar's_variational_principle
Ratio in stellar astrophysics
In stellar astrophysics, the Schönberg–Chandrasekhar limit is the maximum mass of a non-fusing, isothermal core that can support an enclosing envelope
Schönberg–Chandrasekhar_limit
Theory of gravitation as curved spacetime
("Eddington luminosity"), see Celotti, Miller & Sciama 1999, observations of stellar dynamics in the center of our own Milky Way galaxy, cf. Schödel et al. 2003
General_relativity
Random motion of particles suspended in a fluid
negligible, individual particle dynamics can be approximated using Brownian dynamics in place of Langevin dynamics. In stellar dynamics, a massive body (star,
Brownian_motion
Academic fields of study or professions
Quantum electrodynamics Relativistic dynamics Stellar dynamics System dynamics Thermodynamics Vehicle dynamics Econophysics Electricity Electromagnetism Electrostatic
Outline of academic disciplines
Outline_of_academic_disciplines
Orbital radius at which a satellite might break up due to gravitational force
Ellipsoidal configurations of equilibrium". Problems of cosmogony and stellar dynamics. Discussion of the Roche Limit; Archived 2019-09-16 at the Wayback
Roche_limit
Approximation algorithm for the n-body problem
body and the algorithm degenerates to a direct-sum algorithm. NEMO (Stellar Dynamics Toolbox) Nearest neighbor search Fast multipole method References Pfalzner
Barnes–Hut_simulation
Branch of the American Astronomical Society
mechanics, solar system dynamics, stellar dynamics, as well as the dynamics of the interstellar medium and galactic dynamics, and coordination of such
Division on Dynamical Astronomy
Division_on_Dynamical_Astronomy
Flow of gas ejected from the upper atmosphere of a star
A stellar wind is a flow of gas ejected from the upper atmosphere of a star. It is distinguished from the bipolar outflows characteristic of young stars
Stellar_wind
Hypothetical process of mining a star for resources
significantly shorter lifespan than small ones. Current theories of stellar dynamics also suggest that there is very little mixing between the bulk of a
Star_lifting
Energy driving the accelerated expansion of the universe
2023). "No, black holes are not the source of dark energy". Stars, Stellar Dynamics, Black Holes, and Gravitational Waves at UNC. Chapel Hill, NC: University
Dark_energy
Small number of stars that orbit each other
A star system or stellar system is a small number of stars that orbit each other, bound by gravitational attraction. It may sometimes be used to refer
Star_system
Gravitational force holding a body or system of bodies together
change. Nature 409, p. 1026-1029. February 22, 2001. Lynden-Bell, D. Stellar dynamics: Exact solution of the self-gravitation equation. Monthly Notices of
Self-gravitation
David; Alexander, Tal; Mikkola, Seppo; Will, Clifford (August 2011). "Stellar dynamics of extreme-mass-ratio inspirals". Physical Review D. 84 (4) 044024
Extreme_mass_ratio_inspiral
French mathematician and astronomer (1931–2013)
Observatory. In astronomy, Hénon is well known for his contributions to stellar dynamics. In the late 1960s and early 1970s he made important contributions
Michel_Hénon
Grouping of stars by similar metallicity
1944, Walter Baade categorized groups of stars within the Milky Way into stellar populations. In the abstract of the article by Baade, he recognizes that
Stellar_population
Black hole formed by a collapsed star
A stellar black hole (or stellar-mass black hole) is a black hole formed by the gravitational collapse of a star. They have masses ranging from about five
Stellar_black_hole
Changed position of star vs background
Stellar parallax is the apparent shift of position (parallax) of any nearby star (or other object) against the background of distant stars. By extension
Stellar_parallax
Armenian physicist (born 1955)
are chaos in non-linear systems, accretion onto massive black holes, stellar dynamics, and observational cosmology. Gurzadyan has papers predicting elliptical
Vahe_Gurzadyan
Estonian astronomer
1988) was an Estonian astronomer, who worked mainly in the field of stellar dynamics. Grigori Kuzmin was born in 1917 in Viipuri, part of the Grand Duchy
Grigori_Kuzmin
Outermost layer of a star's atmosphere
Scientists have greater access to the solar corona than they do to other stellar coronae, since it is inside our solar system. This means that the coronae
Stellar_corona
Globular cluster in the constellation Centaurus
Merritt, David; Meylan, Georges; Mayor, Michel (September 1997). "The stellar dynamics of Omega Centauri". The Astrophysical Journal. 114: 1074–1086. arXiv:astro-ph/9612184
Omega_Centauri
Fluctuations in stellar radius
speaking, the dynamics has a center manifold, or more precisely a near center manifold. In addition, it has been found that the stellar pulsations are
Stellar_pulsation
Branch of modern astronomy
astrophysical fluid dynamics include dynamics of stellar systems, accretion disks, astrophysical jets, Newtonian fluids, and the fluid dynamics of galaxies.
Astrophysical_fluid_dynamics
Large self-illuminated object in space
star catalogues that identify the known stars and provide standardized stellar designations. The observable universe contains an estimated 1022 to 1024
Star
Type of emission nebula created by dying red giants
Grigor A. (1997), The Physics and dynamics of planetary nebulae, Springer, ISBN 978-3-540-60965-0 Harpaz, Amos (1994), Stellar Evolution, A K Peters, Ltd.,
Planetary_nebula
Classification in astronomy
Since most compact object types represent endpoints of stellar evolution, they are also called stellar remnants, and accordingly may be called dead stars
Compact_object
Czech astronomist (1919–2020)
and earned his DSc in Astronomy in 1961. He published 44 papers on stellar dynamics and planetary nebulae and 80 papers and articles on the geostationary
Luboš_Perek
Type of gravitational orbit seen in triaxial systems
In stellar dynamics, a box orbit refers to a particular type of orbit that can be seen in triaxial systems, i.e. systems that do not possess a symmetry
Box_orbit
Methods and computing tools developed and used in astrophysics research
magnetohydrodynamics, astrophysical radiative transfer, stellar and galactic dynamics, and astrophysical fluid dynamics. A recently developed field with interesting
Computational_astrophysics
Galaxy in the constellation Leo
Lucey, J. R.; Edge, A. C. (2017). "Stellar dynamics in the strong-lensing central galaxy of Abell 1201: A low stellar mass-to-light ratio a large central
Abell_1201_BCG
Observatory
paper on stellar dynamics in which he hypothesized that the star streams discovered by Kapteyn arose from a Maxwellian distribution of stellar velocities
Royal Observatory, Cape of Good Hope
Royal_Observatory,_Cape_of_Good_Hope
Globular cluster in the constellation Tucana
McLaughlin, D.E.; et al. (2006). "Hubble Space Telescope Proper Motions and Stellar Dynamics in the Core of the Globular Cluster 47 Tucanae". Astrophysical Journal
47_Tucanae
luminosity. stellar designation stellar dynamics stellar envelope 1. The region within the volume of a star that transports energy from the stellar core to
Glossary_of_astronomy
Early stage in the process of star formation
its parent molecular cloud. It is the earliest phase in the process of stellar evolution. For a low-mass star (i.e. that of the Sun or lower), it lasts
Protostar
Dwarf galaxy in the constellation Leo
the past. In the work published in 2025 the authors claim that the stellar dynamics of Segue 1 are best modeled by a point-like mass in its center with
Segue_1
Gravitational process studied in astronomy
within molecular clouds in interstellar space—sometimes referred to as "stellar nurseries" or "star-forming regions"—collapse and form stars. As a branch
Star_formation
Changes to stars over their lifespans
Stellar evolution is the process by which a star changes over the course of time. Depending on the mass of the star, its lifetime can range from a few
Stellar_evolution
Norwegian astronomer (1934–2024)
2021. Retrieved 27 June 2012. "Sverre Aarseth, father of open source stellar dynamics software, has passed on to a higher orbit – ASCL.net". 7 January 2025
Sverre_Aarseth
Galaxy in the constellation Perseus
of van den Bosch, but with higher spatial resolution. After using stellar dynamics and luminosity models to estimate the mass of the black hole, they
NGC_1277
Australian astronomer known for work on galaxy structure and supermassive black holes
doi:10.1146/annurev-astro-082214-122432. Alexander, Tal (2017). "Stellar Dynamics and Stellar Phenomena Near a Massive Black Hole". Annual Review of Astronomy
Alister_W._Graham
Set of non-stellar objects in orbit around a star
A planetary system consists of a set of non-stellar bodies which are gravitationally bound to and in orbit of a star or star system. Generally speaking
Planetary_system
Creation of chemical elements within stars
In astrophysics, stellar nucleosynthesis is the creation of chemical elements by nuclear fusion reactions within stars. Stellar nucleosynthesis has occurred
Stellar_nucleosynthesis
Galaxy in the constellation Ursa Major
one has mass of approximately 3 × 107 solar masses, as measured from stellar dynamics. In April 2010, radio astronomers working at the Jodrell Bank Observatory
Messier_82
American physicist, writer, and novelist (born 1948)
gravitation theory, the structure and behavior of accretion disks, stellar dynamics, radiative processes, and relativistic plasmas. Some of his significant
Alan_Lightman
Central object of a galaxy
Core collapse (cluster) Galactic Center Stellar dynamics Böker 2010a, p. 61. Merritt, David (2013). Dynamics and Evolution of Galactic Nuclei. Princeton
Central_massive_object
Structure of stars
Stellar structure models describe the internal structure of a star in detail and make predictions about the luminosity, the color and the future evolution
Stellar_structure
Astrophysics accretion disc criterion
focused primarily on the gas-dominated component, the inclusion of stellar dynamics is essential for interpreting the stability of more evolved or massive
Toomre's_stability_criterion
Hypothetical class of star that develops from a red dwarf
Simulations have been conducted on the future evolution of red dwarfs with stellar mass between 0.06 M☉ and 0.25 M☉. Of the masses simulated, the bluest of
Blue_dwarf_(red-dwarf_stage)
Scatter plot of stars showing the relationship of luminosity to stellar classification
relationship between the stars' absolute magnitudes or luminosities and their stellar classifications or effective temperatures. It is also sometimes called
Hertzsprung–Russell_diagram
Kazakhstan research institute
stars, and active galaxies. The topics of theoretical research include stellar dynamics and computational astrophysics, active galactic nuclei, cosmology,
Fesenkov Astrophysical Institute
Fesenkov_Astrophysical_Institute
Observatory
celestial bodies, small bodies of the Solar System, star catalogs and stellar dynamics, as well as gravitational lenses. The astronomical observatory is subordinate
Kharkiv_Observatory
Stars with a supergiant luminosity class with a spectral type of K or M
(RSGs) are stars with a supergiant luminosity class (Yerkes class I) and a stellar classification K or M. They are the largest stars in the universe in terms
Red_supergiant
American astrophysicist
Celestial and Stellar Dynamics. Barbara Ryden, 2025, Cambridge, England: Cambridge University Press ISBN 978-1-108-81901-5 Astrophysical Gas Dynamics. Barbara
Barbara_Ryden
English physicist, astronomer, and mathematician (1877–1946)
Press. 2009 [1926]. ISBN 978-1-108-00563-0. Problems of Cosmology and Stellar Dynamics. Cambridge University Press. 2009 [1919]. ISBN 978-1-108-00568-5. The
James_Jeans
Problem in physics and celestial mechanics
Dynamics. Cambridge: Cambridge University Press. ISBN 978-0-521-77303-4. Heggie, Douglas C. (1991). "Chaos in the n-body Problem of Stellar Dynamics"
N-body_problem
Curve on the Hertzsprung-Russell diagram representing stars of a particular age
In stellar evolution, an isochrone is a curve on the Hertzsprung-Russell diagram, representing a population of stars of the same age but with different
Stellar_isochrone
Gold medal awarded annually by the Institute of Physics
quantum nature of materials" 2023 James Binney "advancing the science of stellar dynamics and using strong physical intuition to widen and deepen our understanding
Isaac_Newton_Medal
Relative abundance of heavy elements in a star or other astronomical object
nonmetals in chemistry. The presence of heavier elements is the result of stellar nucleosynthesis. The majority of elements that are heavier than hydrogen
Metallicity
Galaxy in the constellation Perseus
a Supermassive Black Hole in the Galaxy NGC 1023 from the Nuclear Stellar Dynamics". The Astrophysical Journal. 550 (1): 75–86. arXiv:astro-ph/0011204
NGC_1023
Spherical collection of stars
Dynamical Evolution of Globular Clusters. The Use of Supercomputers in Stellar Dynamics, Proceedings of a Workshop Held at the Institute for Advanced Study
Globular_cluster
Methods for estimating the age of a star
in stellar age estimation, an attempt to identify within reasonable degrees of confidence what the age of a star is. These methods include stellar evolutionary
Stellar_age_estimation
center, arXiv:0903.2912 phiGRAPE, an N-body code optimized for GRAPE clusters How to build and use special purpose PC clusters in stellar dynamics v t e
GravitySimulator
Swiss astronomer
cosmology. First, he studied the internal stellar kinematics and dynamics of globular clusters, which are stellar systems containing from a few 105 to a
Georges_Meylan
Calculated property of a star or planet
luminosity of a star is then L = 4πR2σTeff4, where R is the stellar radius. The definition of the stellar radius is obviously not straightforward. More rigorously
Effective_temperature
Armenian astronomer (1922–2014)
research topics are: the chaos in non-linear systems, N-body dynamics, stellar dynamics, Cosmic Microwave Background radiation, observational cosmology
Grigor_Gurzadyan
decomposition method Tateos Agekian, astrophysicist, one of the pioneers of Stellar Dynamics Hagop S. Akiskal, psychiatrist best known for his pioneering research
Lists_of_Armenians
System of units used for N-body simulations
scales". In Hut, P.; McMillan, S. (eds.). The Use of Supercomputers in Stellar Dynamics. Lecture Notes in Physics. Vol. 267. pp. 233–235. Bibcode:1986LNP.
N-body_units
Branch of astronomy using gravitational waves
1088/0264-9381/29/12/124016. S2CID 54822413. Amaro-Seoane, P. (May 2012). "Stellar dynamics and extreme-mass ratio inspirals". Living Reviews in Relativity. 21
Gravitational-wave_astronomy
Dim, low mass stars on the main sequence
definition is synonymous with stellar M dwarfs, yielding a maximum temperature of 3,900 K and 0.6 M☉. Another includes all stellar M-type main-sequence and
Red_dwarf
Region at the center of a star
A stellar core is the extremely hot, dense region at the center of a star. For an ordinary main sequence star, the core region is the volume where the
Stellar_core
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