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Accumulation of particles into a massive object by gravitationally attracting more matter
In astrophysics, accretion is the accumulation of matter into a massive object by gravitationally attracting more matter. If the matter is gaseous the
Accretion_(astrophysics)
Structure formed by diffuse material in orbital motion around a massive central body
Accretion disks are a ubiquitous phenomenon in astrophysics; active galactic nuclei, protoplanetary disks, and gamma ray bursts all involve accretion
Accretion_disk
Topics referred to by the same term
Look up accretion in Wiktionary, the free dictionary. Accretion may refer to: Accretion (astrophysics), the formation of planets and other bodies by collection
Accretion
Model for the accretion of a uniform gas by a massive body
Bondi–Hoyle–Lyttleton (BHL) accretion (also known as Bondi–Hoyle accretion) is a mathematical model for the accretion of a uniform gas by a massive body
Bondi–Hoyle–Lyttleton accretion
Bondi–Hoyle–Lyttleton_accretion
Astronomical theory about the Solar System
(August 2012). "Rapid growth of gas-giant cores by pebble accretion". Astronomy & Astrophysics. 544: A32. arXiv:1205.3030. Bibcode:2012A&A...544A..32L.
Nebular_hypothesis
Accretion of matter within the interstellar medium
In astrophysics, the Bondi accretion, named after Hermann Bondi, is spherical accretion onto a compact object traveling through the interstellar medium
Bondi_accretion
Type of supernova in binary systems
process, the white dwarf would collapse to form a neutron star, in an accretion-induced non-ejective process, as normally occurs in the case of a white
Type_Ia_supernova
Subfield of astronomy
Quasar exemplifying supermassive black hole seed growth. Accretion (astrophysics) Accretion disks Astrophysical jets and outflows Stellar flares and coronal
Outline_of_astrophysics
Compact astronomical body
(2005). "Super-Eddington Black Hole Accretion". Growing Black Holes: Accretion in a Cosmological Context. ESO Astrophysics Symposia. pp. 257–273. doi:10.1007/11403913_49
Black_hole
Largest type of black hole
Andrew; Raine, Derek J. (January 2002). "Accretion Power in Astrophysics: Third Edition". Accretion Power in Astrophysics. Cambridge, UK: Cambridge University
Supermassive_black_hole
Gravitationally-binding region around a star in a binary system
Philipp (February 2014). "The evolution of binary systems". Accretion Processes in Astrophysics. pp. 45–88. doi:10.1017/CBO9781139343268.003. ISBN 9781139343268
Roche_lobe
Net movement of mass from one location, phase, etc. to another
McCabe–Thiele method Vapor–liquid equilibrium Liquid–liquid extraction Separation process Binary star Type Ia supernova Thermodiffusion Accretion (astrophysics)
Mass_transfer
Class of binary stars
is typically around 15 to 20. The brightest part of the system is the accretion disk around the compact object. The orbital periods of LMXBs range from
X-ray_binary
Pulsar with a rotational period less than about 10 milliseconds
rapidly rotating neutron stars that have been spun up or "recycled" through accretion of matter from a companion star in a close binary system. For this reason
Millisecond_pulsar
Gas and dust surrounding a newly formed star
The protoplanetary disk may not be considered an accretion disk; while the two are similar, an accretion disk is hotter and spins much faster, accreting
Protoplanetary_disk
Astrophysical limit on radiation from stars
2004). "Growth of massive black holes by super-Eddington accretion". Astronomy & Astrophysics. 420 (3): L23–L26. arXiv:astro-ph/0405024. doi:10.1051/0004-6361:20040157
Eddington_luminosity
Miniature analogue of a quasar caused by black hole accretion
matter being pulled from the companion star forms an accretion disk around the black hole. This accretion disk may become so hot, due to friction, that it
Microquasar
Accumulation of particles into planetesimals
Pebble accretion is the accumulation of particles, ranging from centimeters up to meters in diameter, into planetesimals in a protoplanetary disk that
Pebble_accretion
Astrophysical theory
physicist John Papaloizou and James E. Pringle which proposes that tori, or accretion disks, in anisotropic stellar systems with constant specific angular momentum
Papaloizou–Pringle instability
Papaloizou–Pringle_instability
Theory about supermassive black holes
now fully integrated into modern understanding of astrophysics including the model that accretion disks are supported by magnetic fields, that extragalactic
Sołtan_argument
Solid objects in protoplanetary disks and debris disks
and protoplanets continue to grow (faster than planetesimals). Accretion (astrophysics) Disrupted planet List of interstellar and circumstellar molecules
Planetesimal
Pulling apart of a star by tidal forces
Some portion of the stellar material is captured into orbit, forming an accretion disk around the black hole, which emits electromagnetic radiation. In
Tidal_disruption_event
Type of interstellar cloud
molecular cloud Perseus molecular cloud Accretion (astrophysics) Astrochemistry Atomic and molecular astrophysics Cosmic dust Cosmochemistry Evaporating
Molecular_cloud
Fluid layer between Earth's solid inner core and its mantle
the water delivery to terrestrial embryos by ice pebble accretion". Astronomy & Astrophysics. 589: A15. arXiv:1512.02414. Bibcode:2016A&A...589A..15S
Earth's_outer_core
Rotational center of the Milky Way galaxy
black hole at the center of the Milky Way. Accretion of gas onto the black hole, probably involving an accretion disk around it, would release energy to
Galactic_Center
Hot plasma around an accretion disk
high-energy astrophysics, an accretion disk corona (ADC) is a region of hot plasma surrounding an accretion disk, analogous to a stellar corona. Accretion disk
Accretion_disk_corona
Galaxy with an annular appearance
via Astrophysics Data System. Finkelman, Ido; Moiseev, Alexei; Brosch, Noah; Katkov, Ivan (2011-12-11). "Hoag's Object: evidence for cold accretion on
Ring_galaxy
unusually strong outburst (increase in brightness) caused by an increased accretion rate. The period of the superhump variations can be either greater or
Superhump
Supermassive black hole at the center of the Milky Way
radio source. In May 2022, astronomers released the first image of the accretion disk around the event horizon of Sagittarius A*, using the Event Horizon
Sagittarius_A*
Russian astrophysicist
relativistic astrophysics department at the Sternberg Astronomical Institute, Moscow University. As a well-known specialist in the theory of accretion disks
Nikolai_Shakura
Construct in astrophysics
birthline depends in detail on the accretion rate and geometry, i.e. whether or not it is occurring through an accretion disk. This means that the birthline
Stellar_birthline
Distance from a young star where ice forms
carbon monoxide to condense into solid grains, which will allow their accretion into planetesimals. Beyond the line, otherwise gaseous compounds (which
Frost_line_(astrophysics)
Large planetary embryo
candidates are known and some detections were later questioned. Accretion (astrophysics) Fusor (astronomy) Mesoplanet Planetesimal Crespi, Samuele; Dobbs-Dixon
Protoplanet
Active galactic nucleus (AGN) containing a supermassive black hole
by accretion onto a supermassive black hole with a mass ranging from millions to tens of billions of solar masses, surrounded by a gaseous accretion disc
Quasar
Concept in astrophysics regarding radiation transparency
Optical depth in astrophysics refers to a measure of transparency for electromagnetic radiation within an astrophysical medium. Quantified by the symbol
Optical_depth_(astrophysics)
Type of binary star
the accretion of stellar wind from the massive star onto the compact object. Because massive stars have powerful stellar winds, the X-ray accretion luminosity
High-mass_X-ray_binary
Research institute located in Garching, Germany
astronomy and astrophysics, including supermassive black holes, galaxy clusters, active galactic nuclei and quasars, X-ray binaries, and accretion discs; Stellar
Max Planck Institute for Astrophysics
Max_Planck_Institute_for_Astrophysics
Stellar core remnant
is theorised to happen: stable accretion of material from a companion, the collision of two white dwarfs, or accretion that causes ignition in a shell
White_dwarf
Merging of droplets, bubbles or particles
collision rate are the droplet concentration and turbulence. Accretion (astrophysics) Accretion (meteorology) Bergeron process Coalescer Postema M, Marmottant
Coalescence_(physics)
Soviet astronomer (1917–1999)
Planets. Moscow: Nauka Press, 1969. Trans. NASA TTF 677, 1972. Accretion (astrophysics) George Wetherill Schmadel, Lutz D. (2003). Dictionary of Minor
Viktor_Safronov
English astronomer and mathematician (1904–1999)
won the Gold Medal of the Royal Astronomical Society in 1976. Accretion (astrophysics) History of Solar System formation and evolution hypotheses Mestel
William_McCrea_(astronomer)
Type of planet
giant and mass transfers from it to an accretion disk around the other star where the planet can form. This accretion disk is referred to by the name second-generation
Second_generation_planet
American astrophysicist
Abramowicz [pl; sv]. Blaes' dissertation was titled The Stability of Thick Accretion Disks. Blaes was the Chaim Weizmann Research Fellow in Theoretical Physics
Omer_Blaes
Russian-American computational astrophysicist
rotation axis of the accretion disks of black holes. She works as a senior research associate in the Cornell Center for Astrophysics and Planetary Science
Marina_Romanova
Type of nuclear fusion that occurs at high densities & low temperatures
dynamicity can be cancelled out. Cold fusion Thermonuclear reaction Accretion (astrophysics) Plasma (physics) Quantum tunnelling Afanasjev, A.V.; Gasques,
Pycnonuclear_fusion
Binary star system in the constellation Reticulum
explain extreme Be depletion in solar-like stars: accretion or rotation effects?". Astronomy & Astrophysics. 546: 7. arXiv:1209.1812. Bibcode:2012A&A...546A
Zeta_Reticuli
Quasar
supermassive black hole feeding on intensely hot gas and matter in an accretion disc. Given its observed redshift of 2.219, the light travel time of TON
TON_618
Hypothetical early-universe star with a black hole core
thick accretion disk or a quasi-spherical accretion, with at least 10−4 to several M☉ per year, possibly up to a highly super-Eddington accretion rate
Quasi-star
Compact region at a galaxy's center with abnormally high luminosity
The non-stellar radiation from an AGN is theorized to result from the accretion of matter by a supermassive black hole at the center of its host galaxy
Active_galactic_nucleus
X-ray binary in Cygnus containing a stellar black hole
Earth to the Sun. A stellar wind from the star provides material for an accretion disk around the X-ray source. Matter in the inner disk is heated to millions
Cygnus_X-1
Award
supports, and recognizes scientists for outstanding work in the fields of astrophysics, nanoscience and neuroscience. Three prizes are awarded every second
Kavli_Prize
American astrophysicist
was titled Using black hole x-ray binaries as laboratories for probing accretion disk theory in strong gravity. He was a postdoctoral fellow in the school
Shane_Davis_(astrophysicist)
Astrophysics shock waves
collision between molecular clouds or by a gravitational collapse of a cloud. Accretion shocks at the edge of galaxy clusters. Zel'dovich, Yakov Porisovich; Raizer
Shock_waves_in_astrophysics
Physics, Theoretical Physics, Environmental Physics and Theoretical Astrophysics. The Kirchhoff-Institut für Physik (Kirchhoff Institute of Physics, KIP)
Heidelberg University Faculty of Physics and Astronomy
Heidelberg_University_Faculty_of_Physics_and_Astronomy
NASA space telescope of the Explorer program
PRIMA (PRobe far-Infrared Mission for Astrophysics) is a planned NASA far-infrared space telescope scheduled to launch in 2033. The spacecraft will be
PRIMA_(spacecraft)
Methods and computing tools developed and used in astrophysics research
Computational astrophysics refers to the methods and computing tools developed and used in astrophysics research. Like computational chemistry or computational
Computational_astrophysics
Type of astronomical binary system
fills its Roche lobe and the compact object begins to accrete off of it. Accretion from an LMXB produces bright X-ray emission that can be observed by astronomers
Low-mass_X-ray_binary
Line describing path of matter near a black hole
stretch) is a traversal line describing the path matter takes through the accretion disc of a black hole. A tendex line typically follows a spiral around
Tendex_line
T Tauri-type star in the constellation Centaurus
protoplanetary disk PDS 70. A spiral accretion stream and a potential third protoplanet". Astronomy and Astrophysics. 685: L1. arXiv:2403.04855. Bibcode:2024A&A
PDS_70
Class of astronomical objects
its stellar wind, which flows onto the hot compact star, usually via an accretion disk. Symbiotic binaries are of particular interest to astronomers as
Symbiotic_binary
Periodic modulation of stellar accretion rate
Muzerolle, James; et al. (2013), "Pulsed accretion in a variable protostar", Astrophysics. Solar and Stellar Astrophysics (in German), vol. 493, no. 7432, pp
Pulsed_accretion
Process of creating new atomic nuclei from existing nucleons
from Black Hole Accretion Disks" (PDF). Archived (PDF) from the original on 2016-09-10. Frankel, N. (2017). Nucleosynthesis in Accretion Disks Around Black
Nucleosynthesis
Large, round non-stellar astronomical object
Ceres: Coupling of accretion with compaction by creep and implications for the water-rock differentiation" (PDF). Astronomy & Astrophysics. 584: A117. Bibcode:2015A&A
Planet
Indian-American theoretical astrophysicist
contributions to theoretical astrophysics, specifically to high-energy astrophysics. He wrote landmark studies on gamma-ray bursts, accretion disks, black holes
Ramesh Narayan (astrophysicist)
Ramesh_Narayan_(astrophysicist)
Highly magnetic type of cataclysmic variable binary star system
SDSS. VI. SDSS J120615.73+510047.0: a new low accretion rate magnetic binary". Astronomy and Astrophysics. 500 (2): 867–872. arXiv:0903.5417. Bibcode:2009A&A
Polar_(star)
Planet larger than Neptune but smaller than Saturn
Saturn (20-100 M🜨, 4-8 R🜨, 0.687-1.64 g/cm3). According to the core-accretion model of planet formation, most planets that reach a ~20 M🜨 threshold
Super-Neptune
Formation processes of the planet Jupiter
the Sun’s formation, quickly reaching its current mass of 318 M⊕. The accretion process of the planet was mediated by the formation of a circumplanetary
Formation_of_Jupiter
Stars with irregular large fluctuations in brightness
forms in most cases an accretion disk around the white dwarf. Strong UV and X-ray emission is often detected from the accretion disc, powered by the loss
Cataclysmic_variable_star
Binary star system in the constellation Aquila
companion star which rapidly loses mass into an accretion disc formed around the central object. The accretion disc is subject to extreme heating as it spirals
SS_433
Free-floating planet in the constellation Leo
magnetic activity and/or weak accretion. The team also found emission due to neutral helium (He), which is another sign of accretion. Observations with the VLT
2MASS_J11151597+1937266
System of stars and interstellar matter
Bournaud, F.; Combes, F. (2002). "Gas accretion on spiral galaxies: Bar formation and renewal". Astronomy & Astrophysics. 392 (1): 83–102. arXiv:astro-ph/0206273
Galaxy
Long-period exoplanet orbiting b Centauri
uncertain. It is believed that most giant planets are formed via core accretion, in which a rocky core, after growing to a critical mass, starts rapidly
B_Centauri_b
Plasma that cosmologists believe exists between galaxies
nuclei, along with the gravitationally-driven processes of merging and accretion. Part of the gravitational energy supplied by these effects is converted
Warm–hot_intergalactic_medium
Class of active galaxies with very bright nuclei
Astronomy and Astrophysics. 305: 53. arXiv:astro-ph/9504093. Bibcode:1996A&A...305...53B. Mathur, S.; Grupe, D. (2005). "Black hole growth by accretion". Astronomy
Seyfert_galaxy
B-type star with forbidden emission lines
Carinae, the secondary star accretes part of the primary wind into a curved accretion tail. Near periastron, the orbital motion causes the primary star and
B(e)_star
Shock wave caused by blowing stellar wind
In astrophysics, bow shocks are shock waves in regions where the conditions of density and pressure change dramatically due to blowing stellar wind. Bow
Bow_shock
Stream of ionized matter flowing away from a rotating astronomical object
believed to arise from dynamic interactions within accretion disks. One explanation is that as an accretion disk spins, it generates a rotating, tangled magnetic
Astrophysical_jet
Binary star system in the Phoenix constellation
Halpha emission and signs of accretion in a circumbinary planetary mass companion from MUSE". Astronomy and Astrophysics. 638: L6. arXiv:2005.11725. Bibcode:2020A&A
Delorme_1
Galaxy containing the Solar System
estimated mass of 4.1–4.5 million times the mass of the Sun. The rate of accretion of the SMBH is consistent with an inactive galactic nucleus, being estimated
Milky_Way
Multiple star system in the constellation of Lyra
(2018). "Physical properties of β Lyrae a and its opaque accretion disk". Astronomy and Astrophysics. 618: A112. arXiv:1807.04789. Bibcode:2018A&A...618A
Beta_Lyrae
Type of neutron star with beams of radiation
Pranab (April 2007). Rotation and Accretion Powered Pulsars. World Scientific Series in Astronomy and Astrophysics. Vol. 10. World Scientific. p. 2. Bibcode:2007rapp
Pulsar
Research facility for astrophysics in Germany
Leibniz Institute for Astrophysics Potsdam (AIP) is a German research institute. It is the successor of the Berlin Observatory founded in 1700 and of the
Leibniz Institute for Astrophysics Potsdam
Leibniz_Institute_for_Astrophysics_Potsdam
Explanation for how quasars are powered
Frank, Juhan; King, Andrew; Raine, Derek J. (February 2002). Accretion Power in Astrophysics (Third ed.). Cambridge, UK: Cambridge University Press. Bibcode:2002apa
Blandford–Znajek_process
Astrophysics accretion disc criterion
relationship between parameters of a differentially rotating, gaseous accretion disc which can be used to determine approximately whether the system is
Toomre's_stability_criterion
Type of low-mass X-ray binary
shape of its X-ray color-color diagram. Z-sources have high rates of accretion, typically more than 50% of the Eddington limit, and relatively strong
Z_source
Property of accretion disks
In accretion disk physics, geometrical thickness is a property of an accretion disk representing the relative vertical scale height (thickness) of the
Geometrical_thickness
Wolf–Rayet star in the constellation Dorado
formation by accretion from molecular clouds predict an upper limit to the mass a star can achieve before its radiation prevents further accretion. The most
R136a1
S.; Mayer, L.; Zwick, L. (2021). "Maximum accretion rate of supermassive stars". Astronomy & Astrophysics. 652: L7. arXiv:2105.13373. Bibcode:2021A&A
List_of_largest_stars
Nuclear explosion in a white dwarf star
ignition, as in the star T Coronae Borealis. Under certain conditions, mass accretion can eventually trigger runaway fusion that destroys the white dwarf rather
Nova
Star system in the Centaurus constellation
be possible if they formed in a dense star cluster), would permit an accretion-friendly environment farther from the star. Bodies around Alpha Centauri
Alpha_Centauri
Israeli astrophysicist
theory of accretion disks applying mathematical approximation methods that were novel to astrophysics. He investigated instabilities of accretion disks that
Oded_Regev_(physicist)
Planet not gravitationally bound to a star
Chauvin, G.; Rojo, P. (2013). "OTS 44: Disk and accretion at the planetary border". Astronomy & Astrophysics. 558 (7): L7. arXiv:1310.1936. Bibcode:2013A&A
Rogue_planet
Large self-illuminated object in space
Morse, J.; Reipurth, B. (1996). "The Birth of Stars: Herbig-Haro Jets, Accretion and Proto-Planetary Disks". In Benvenuti, Piero; Macchetto, F. D.; Schreier
Star
Approximation of black hole gravitational potential
hole accretion. Paczyński, Bohdan; Wiita, Paul J. (August 1980), "Thick accretion disks and supercritical luminosities", Astronomy & Astrophysics, 88:
Paczyński–Wiita_potential
Study of astronomical objects outside the Milky Way Galaxy
which give insight into physical phenomena (e.g. super massive black hole accretion and the presence of dark matter). It is through extragalactic astronomy
Extragalactic_astronomy
Very compact quasi-stellar radio source
research in astronomy and high-energy astrophysics. Blazar research includes investigation of the properties of accretion disks and jets, the central supermassive
Blazar
predicted by standard models? Astrophysical jet: Why do only certain accretion discs surrounding certain astronomical objects emit relativistic jets
List of unsolved problems in physics
List_of_unsolved_problems_in_physics
Region of a star
Maeder, A. (2001). "Formation of massive stars by growing accretion rate". Astronomy and Astrophysics. 373: 190–198. arXiv:astro-ph/0105054. Bibcode:2001A&A
Convection_zone
British theoretical astrophysicist
mechanism for jet formation through hydromagnetic winds launched from accretion disks. In addition to the Blandford–Znajek and Blandford–Payne mechanisms
Roger_Blandford
Nuclear fusion forming a helium-3 nucleus
"Deuterium burning in objects forming via the core accretion scenario". Astronomy & Astrophysics. 547: A105. arXiv:1210.0538. Bibcode:2012A&A...547A
Deuterium_fusion
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