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Structure formed by diffuse material in orbital motion around a massive central body
An accretion disk is a structure (often a circumstellar disk) formed by diffuse material in orbital motion around a massive central body. The central
Accretion_disk
Accumulation of particles into a massive object by gravitationally attracting more matter
into an accretion disk. Most astronomical objects, such as galaxies, stars, and planets, are formed by accretion processes. The accretion model that
Accretion_(astrophysics)
Astronomical theory about the Solar System
protoplanetary disk evolving into a planetary system over the next 10–100 million years. The protoplanetary disk is an accretion disk that feeds the central
Nebular_hypothesis
Gas and dust surrounding a newly formed star
Ae/Be 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
Protoplanetary_disk
Compact astronomical body
such as visible light. Matter falling toward a black hole can form an accretion disk of infalling plasma, heated by friction and emitting light. In extreme
Black_hole
Accumulation of matter around a star
A circumstellar disc (or circumstellar disk) is a torus-, pancake- or ring-shaped accretion disk of matter composed of gas, dust, planetesimals, asteroids
Circumstellar_disc
Particle outflow from an accretion disk
astronomy, a disk wind is a particle outflow observed around accretion disks, mainly near protoplanetary disks and active galactic nuclei (AGN). The disk wind
Disk_wind
Galactic X-ray source in the constellation Cygnus that is very likely a black hole
wind from the star provides material for an accretion disk around the X-ray source. Matter in the inner disk is heated to millions of degrees, generating
Cygnus_X-1
Process of creating new atomic nuclei from existing nucleons
Black Hole Accretion Disks" (PDF). Archived (PDF) from the original on 2016-09-10. Frankel, N. (2017). Nucleosynthesis in Accretion Disks Around Black
Nucleosynthesis
2014 film by Christopher Nolan
simulated image of a black hole, praised the warped appearance of the accretion disk but criticized the depiction of the interior of the wormhole and noted
Interstellar_(film)
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*
Accumulation of matter around a planet
Such a disk can manifest itself in various ways. A giant planet will mainly form via core accretion. In this scenario a core forms via the accretion of small
Circumplanetary_disk
Hypothetical planet that orbits a black hole
Blanets are suspected to form in the accretion disk that orbits a sufficiently large black hole, provided the disk is relatively dim. Radiation feedback
Blanet
Largest type of black hole
black hole can reach, while being luminous accretors (featuring an accretion disk), is typically on the order of about 50 billion M☉. However, a 2020
Supermassive_black_hole
Compact region at a galaxy's center with abnormally high luminosity
the central black hole, the rate of gas accretion onto the black hole, the orientation of the accretion disk, the degree of obscuration of the nucleus
Active_galactic_nucleus
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
Very compact quasi-stellar radio source
are captured and spiral into this central black hole, creating a hot accretion disk which generates enormous amounts of energy in the form of photons, electrons
Blazar
Highly magnetic type of cataclysmic variable binary star system
field captures the accretion stream from the donor star before it can develop into an accretion disk. The capture of the accretion stream is known as
Polar_(star)
Miniature analogue of a quasar caused by black hole accretion
forms an accretion disk around the black hole. This accretion disk may become so hot, due to friction, that it begins to emit X-rays. The disk also projects
Microquasar
Measure of a civilization's evolution
photons emitted by the accretion disk. A less exotic means would be to simply capture photons already escaping from the accretion disk, thereby reducing a
Kardashev_scale
Hypothetical hybrid star type
stars may form the population of isolated pulsars with accretion disks. The massive accretion disk may also collapse into a new star, becoming a stellar
Thorne–Żytkow_object
Supernova that ejects a large mass at unusually high velocity
rotating black hole emitting twin astrophysical jets and surrounded by an accretion disk. It is a type of stellar explosion that ejects material with an unusually
Hypernova
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
Free-floating planet in the constellation Leo
a young isolated planetary-mass object that is surrounded by a planetary disk. 2MASS J1115+1937 was discovered in 2017 in the LaTE-MoVeRS survey (Late-Type
2MASS_J11151597+1937266
Early stage in the process of star formation
theoretical effort. This problem is illustrative of the larger issue of accretion disk theory, which plays a role in much of astrophysics. Regardless of the
Protostar
Type of circumstellar disk
Ks-W4>2} , an age of >20 Myr and spectroscopic evidence of accretion. In 2016 volunteers of the Disk Detective project, led by Dr. Steven Silverberg of the
Peter_Pan_disk
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
Class of astronomical objects
stellar wind, which flows onto the hot compact star, usually via an accretion disk. Symbiotic binaries are of particular interest to astronomers as they
Symbiotic_binary
Collapsed core of a massive star
can pull in large amounts of gas from its companion, a process called accretion. These binary systems continue to evolve, with many companions eventually
Neutron_star
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
Type of planet
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 disk as it is
Second_generation_planet
Planetary system consisting of the Sun and objects orbiting it
200 AU and a hot, dense protostar at the center. The planets formed by accretion from this disc, in which dust and gas gravitationally attracted each other
Solar_System
Large, round non-stellar astronomical object
protoplanetary disk. Planets grow in this disk by the gradual accumulation of material driven by gravity, a process called accretion. The word planet
Planet
ring of its accretion disk. The bottom half of the disk is brighter than the top due to Doppler beaming: Material at the bottom of the disk, which is travelling
History_of_black_hole_physics
Class of binary stars
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 ten
X-ray_binary
Astrophysical limit on radiation from stars
Marek A.; Fragile, P. Chris (December 2013). "Foundations of Black Hole Accretion Disk Theory". Living Reviews in Relativity. 16 (1) 1. arXiv:1104.5499. Bibcode:2013LRR
Eddington_luminosity
Rotational center of the Milky Way galaxy
compact gas accretion disk around the central black-hole. Current evidence favors the latter theory, as formation through a large accretion disk is more likely
Galactic_Center
NASA X-ray space telescope of the Explorer program
from the accretion disk winds, NuSTAR and XMM-Newton observed heating and cooling cycles of the relativistic winds leaving the accretion disk. NuSTAR and
NuSTAR
Star whose brightness fluctuates, as seen from Earth
period with the binary orbital period. Instead of forming an accretion disk, the accretion flow is channeled along the white dwarf's magnetic field lines
Variable_star
Gravitational process studied in astronomy
accretion disks. Disk accretion in high-mass protostars, similar to their low-mass counterparts, is expected to exhibit bursts of episodic accretion as
Star_formation
Innermost Galilean moon of Jupiter
contents, and History Star formation Accretion Accretion disk Excretion Capture theory Capture of Triton Circumplanetary disk Circumstellar disc Circumstellar
Io_(moon)
Nebula surrounding a dying star
applied to the PPN context, the accretion disk forms through binary interactions. Magneto-centrifugal launching from the disk surface is then a way to convert
Protoplanetary_nebula
Stellar core remnant
idea is the origin of those planets. Leaving aside formation from the accretion disk surrounding the white dwarf, there are two ways a planet could end in
White_dwarf
Region in spacetime from which nothing can escape
into a black hole. This is not possible. Astronomers can detect only accretion disks around black holes, where material moves with such speed that friction
Event_horizon
Astrophysical technique
continuum, i.e., the light from the accretion disk near the black hole. Put simply, if the brightness of the accretion disk varies, the emission lines, which
Reverberation_mapping
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 is
Pebble_accretion
Largest moon of Uranus
evolution. Like all major moons of Uranus, Titania probably formed from an accretion disk which surrounded the planet just after its formation. Uranus and Neptune
Titania_(moon)
Type of binary star system with a white dwarf and main-sequence star
systems exhibit full accretion disks, while strongly magnetic systems (called polars or AM Herculis systems) exhibit only accretion streams which directly
Intermediate_polar
Fluid instability that causes turbulence in accretion disks
magnetorotational instability (MRI) is a fluid instability that causes an accretion disk orbiting a massive central object to become turbulent. It arises when
Magnetorotational_instability
Branch of astrophysics
formalism originally developed in the field of fluid mechanics. In accretion disks and stellar surfaces, the dense plasma or gas particles collide very
Stellar_dynamics
Small patches of nebulosity associated with newly born stars
entirely understood, but it is believed that interaction between the accretion disk and the stellar magnetic field accelerates some of the accreting material
Herbig–Haro_object
Galaxy in the constellation Virgo
5 ± 0.4 Schwarzschild radii, and is probably powered by a prograde accretion disk around the spinning supermassive black hole. The German-American astronomer
Messier_87
Process of combining atomic nuclei
second. Similar to stellar fusion, extreme conditions within black hole accretion disks can allow fusion reactions. Calculations show the most energetic reactions
Nuclear_fusion
Set of non-stellar objects in orbit around a star
Alternatively, planets may form in an accretion disk of fallback matter surrounding a pulsar. Fallback disks of matter that failed to escape orbit during
Planetary_system
Disk of dust and debris in orbit around a star
Earth has an average distance from the Sun of 1 AU. Accretion disk Asteroid belt Circumplanetary disk – Accumulation of matter around a planet Exoasteroid
Debris_disk
Theoretical stellar remnant
corona Alfvén surface Stellar wind Bubble Bipolar outflow Accretion disk Protoplanetary disk Proplyd Asteroseismology Helioseismology Circumstellar dust
Black_dwarf
Quasar
giant elliptical galaxy with a supermassive black hole and associated accretion disk. It possesses large regions of hot dust and molecular gas, as well as
APM_08279+5255
Hypothesized alternative to a black hole
corona Alfvén surface Stellar wind Bubble Bipolar outflow Accretion disk Protoplanetary disk Proplyd Asteroseismology Helioseismology Circumstellar dust
Gravastar
Planets visible to the naked eye
contents, and History Star formation Accretion Accretion disk Excretion Capture theory Capture of Triton Circumplanetary disk Circumstellar disc Circumstellar
Classical_planet
corona Alfvén surface Stellar wind Bubble Bipolar outflow Accretion disk Protoplanetary disk Proplyd Asteroseismology Helioseismology Circumstellar dust
Lists of stars by constellation
Lists_of_stars_by_constellation
Class of astronomical objects that are X-ray sources
binary star systems and accrete matter from either stellar winds or accretion disks. The accreted matter transfers angular momentum to (or from) the neutron
X-ray_pulsar
Light from the stars
corona Alfvén surface Stellar wind Bubble Bipolar outflow Accretion disk Protoplanetary disk Proplyd Asteroseismology Helioseismology Circumstellar dust
Starlight
Dim, low mass stars on the main sequence
more recently disk winds in NIRCam and NIRSpec observations. The disk wind is an important part in removal of mass from the disk and accretion of material
Red_dwarf
Cataclysmic variable star, consisting of a close binary star system
suggests that dwarf novae result from instability in the accretion disk, when gas in the disk reaches a critical temperature that causes a change in viscosity
Dwarf_nova
Black hole in the constellation Virgo
interactions between the black hole's accretion disk and orbiting objects. For Ansky, researchers suggest a larger debris disk around the black hole, which is
Ansky_(black_hole)
Precession of a gyroscope due to a nearby celestial body's rotation affecting spacetime
deduce the orientation of an accretion disk; a rapidly changing jet orientation suggests a reorientation of the accretion disk, as described above. Exactly
Lense–Thirring_precession
American physicist, writer, and novelist (born 1948)
Douglas Eardley, of a structural instability in orbiting disks of matter, called accretion disks, that form around massive condensed objects such as black
Alan_Lightman
2014 book by Kip Thorne
a Photoreal Feature Scientific concepts The Science of Interstellar Accretion disk Artificial gravity Black hole Supermassive Blanet Blight Bootstrap paradox
The_Science_of_Interstellar
Region just outside event horizons
inspiral, the density of the accretion disk decreases, but it stabilizes afterwards. While inside the plunging region, disk material becomes hotter, aided
Plunging_region
Stellar classification
corona Alfvén surface Stellar wind Bubble Bipolar outflow Accretion disk Protoplanetary disk Proplyd Asteroseismology Helioseismology Circumstellar dust
G-type_main-sequence_star
Two continuous flows of gas from the poles of a star
an accretion disk. The outflow relieves the build-up of angular momentum as material spirals down onto the central star through the accretion disk. The
Bipolar_outflow
Moon of Uranus
partially outside Uranus's magnetosphere. Oberon likely formed from the accretion disk that surrounded Uranus just after the planet's formation. The moon consists
Oberon_(moon)
B-type star with emission lines
observational characteristics of Be stars can now be explained with a gaseous disk that is formed of material ejected from the star. The infrared excess and
Be_star
Region outside of a rotating black hole's event horizon
Blandford–Znajek process Accretion disk Hawking radiation Gravitational lens Microlens Cauchy horizon Mass inflation Bondi accretion M–sigma relation Quasi-periodic
Ergosphere
Dust ring surrounding large stars thousands of solar radii wide
objects might be low-mass stars surrounded by an evaporating protostellar accretion disk. Proplyds were clearly resolved in 1993 using images of the Hubble Space
Proplyd
Relative directions of orbit or rotation
interactions between the star's magnetic field and the planet-forming disk. The accretion disk of the protostar IRAS 16293-2422 has parts rotating in opposite
Retrograde and prograde motion
Retrograde_and_prograde_motion
Type of neutron star with beams of radiation
intermediate polar-type star, where the magnetic field is relatively weak and an accretion disc may form around the white dwarf. The star is in the propeller regime
Pulsar
Planetary nebula in the constellation Draco
something of a mystery. It may suggest the presence of a high temperature accretion disk within a binary star system. The hard X-ray data remain intriguing more
Cat's_Eye_Nebula
Hypothetical class of star that develops from a red dwarf
corona Alfvén surface Stellar wind Bubble Bipolar outflow Accretion disk Protoplanetary disk Proplyd Asteroseismology Helioseismology Circumstellar dust
Blue_dwarf_(red-dwarf_stage)
T-Tauri star
T-Tauri binary that has a planetary-mass companion with a detected accretion disk. SR 12 was discovered by Otto Struve and Mogens Rudkjøbing in 1949 as
SR_12_(star)
Type of direct current electrical generator
1982, p. 87–99 Shatskii, A. A., "Unipolar Induction of a Magnetized Accretion Disk around a Black Hole", (2003) Astronomy Letters, vol. 29, p. 153–157
Homopolar_generator
Stellar classification
star alone. This IR excess is attributable to dust emission from a debris disk where planets form. Surveys indicate massive planets commonly form around
A-type_main-sequence_star
Pulling apart of a star by tidal forces
portion of the stellar material is captured into orbit, forming an accretion disk around the black hole, which emits electromagnetic radiation. In a small
Tidal_disruption_event
Moon of Uranus
This moon, like all regular moons of Uranus, probably formed from an accretion disk that surrounded the planet just after its formation. Umbriel has been
Umbriel
Binary star system in the Phoenix constellation
signs of accretion, despite being 30-45 Myr old, making it similar to Peter Pan disks. These disks show characteristics of a gas-rich disk at unexpected
Delorme_1
Substellar object
Holden, Jonathan; Hyogo, Michiharu (2020-02-01). "Peter Pan Disks: Long-lived Accretion Disks Around Young M Stars". The Astrophysical Journal. 890 (2):
Brown_dwarf
Binary star in the constellation Monoceros
hole in A0620-00 pulls matter from the K-type star into an accretion disk. The accretion disk emits significant amounts of visible light and X-rays. Because
A0620-00
Explanation for how quasars are powered
Generally speaking, it was demonstrated that the power output of the accretion disk is significantly larger than the power output extracted directly from
Blandford–Znajek_process
Central region of the Sun
corona Alfvén surface Stellar wind Bubble Bipolar outflow Accretion disk Protoplanetary disk Proplyd Asteroseismology Helioseismology Circumstellar dust
Solar_core
Star's outer shell from which light is radiated
corona Alfvén surface Stellar wind Bubble Bipolar outflow Accretion disk Protoplanetary disk Proplyd Asteroseismology Helioseismology Circumstellar dust
Photosphere
Class of black holes with a mass range of 100 to 100000 solar masses
galaxy and others nearby, based on indirect gas cloud velocity and accretion disk spectra observations of various evidentiary strength. The gravitational
Intermediate-mass_black_hole
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
Upper bound to the mass of cold, nonrotating neutron stars
Cherepashchuk, Anatol (2002). "Observational Manifestations of Precession of Accretion Disk in the SS 433 Binary System". Space Science Reviews. 102 (1): 23–35
Tolman–Oppenheimer–Volkoff limit
Tolman–Oppenheimer–Volkoff_limit
Hypothetical compact star
corona Alfvén surface Stellar wind Bubble Bipolar outflow Accretion disk Protoplanetary disk Proplyd Asteroseismology Helioseismology Circumstellar dust
Q_star
if it were located at a distance of 10 parsecs, or 32.6 light-years. accretion disk A roughly circular mass of diffuse material in orbit around a central
Glossary_of_astronomy
Erroneous AI-generated content
reality, as a consequence of the no-hair theorem, a black hole without an accretion disk is believed to have no magnetic field.) Fast Company asked ChatGPT to
Hallucination (artificial intelligence)
Hallucination_(artificial_intelligence)
Coming together of two stars
dwarf drawing material off a main sequence or red giant star to form an accretion disc. Much more rarely, a type Ia supernova occurs when two white dwarfs
Stellar_collision
Methods for estimating the age of a star
and luminosity classification system, and the presence of a protoplanetary disk, among others. Nearly all of the methods of determining age require knowledge
Stellar_age_estimation
Continuous band of stars that appears on plots of stellar color versus brightness
corona Alfvén surface Stellar wind Bubble Bipolar outflow Accretion disk Protoplanetary disk Proplyd Asteroseismology Helioseismology Circumstellar dust
Main_sequence
Type of star, larger and brighter than the Sun
corona Alfvén surface Stellar wind Bubble Bipolar outflow Accretion disk Protoplanetary disk Proplyd Asteroseismology Helioseismology Circumstellar dust
Giant_star
ACCRETION DISK
ACCRETION DISK
Male
Egyptian
, Horus, the winged disk of the sun.
Male
Egyptian
, disk.
Boy/Male
Australian, Egyptian
Sun Disk
Male
Egyptian
, the spirit of Aton, or the Sun-disk.
Girl/Female
Tamil
Image, Reflection, Also referred to as the disk of brightness surrounding the Sun, Moon
Male
Egyptian
, the most lovely Disk.
Male
Egyptian
, glory of the Solar Disk.
Male
Egyptian
, the spirit of Aten, or the Sun-disk.
Boy/Male
Hindu, Indian, Modern, Sanskrit
Dancer
Girl/Female
Indian
Image, Reflection, Also referred to as the disk of brightness surrounding the Sun, Moon
ACCRETION DISK
ACCRETION DISK
Boy/Male
Muslim
Power
Girl/Female
Greek Italian
Boy/Male
Tamil
Gavaskar | காவஸà¯à®•à®°Â
Girl/Female
Tamil
Girl/Female
Hindu
Belongs to music terms, Melody
Girl/Female
Greek
Sound. A mythological nymph who faded away until only her voice was left.
Girl/Female
Muslim
Success
Girl/Female
Arabic, Australian, Muslim
A Woman who Abstains; Captivating
Girl/Female
Hindu, Indian
Beautiful; The One to whom Money Comes Attracted
Boy/Male
Sikh
Supreme Lord
ACCRETION DISK
ACCRETION DISK
ACCRETION DISK
ACCRETION DISK
ACCRETION DISK
n.
The act of increasing by natural growth; esp. the increase of organic bodies by the internal accession of parts; organic growth.
n.
Corrosive or injurious accretion or influence.
v. i.
To grow larger by accretion; to increase.
n.
Gain to an heir or legatee, failure of a coheir to the same succession, or a co-legatee of the same thing, to take his share.
n.
That which promotes secretion.
n.
A growing together of parts naturally separate, as of the fingers toes.
n.
Continuous growth; an accretion.
n.
The act of increasing, or the matter added, by an accession of parts externally; an extraneous addition; as, an accretion of earth.
n.
The adhering of property to something else, by which the owner of one thing becomes possessed of a right to another; generally, gain of land by the washing up of sand or sail from the sea or a river, or by a gradual recession of the water from the usual watermark.
v. t.
To separate from the blood and elaborate by the process of secretion; to elaborate and emit as a secretion. See Secretion.
n.
The act of secreting or concealing; as, the secretion of dutiable goods.
n.
Free excretion of urine.
n.
Concretion; coherence of separate particles; as, the accretion of particles so as to form a solid mass.
n.
That which is excreted; excretion.
a.
Characterized by accretion; made up; as, accrete matter.
n.
Complete stoppage of a natural secretion or excretion; as, suppression of urine; -- used in contradiction to retention, which signifies that the secretion or excretion is retained without expulsion.
n.
The act of adding; application; accretion.
a.
Relating to accretion; increasing, or adding to, by growth.
a.
Causing secretion; -- said of nerves which go to glands and influence secretion.
n.
The act of accruing; accretion; as, title by accruer.