Astrophysics (Index)About

protoplanetary disk

(PPD, disk, planetary disk, proto-planetary disk, preplanetary disk, PP disk)
(disk of dust and gas around a young star or protostar)

A protoplanetary disk (aka preplanetary disk, either abbreviated PP disk or PPD) is a circumstellar disk, consisting of dust and gas orbiting a young star or protostar such as a T-Tauri star. Radii can be as much as 1000 AU. Such disks are thought to provide the material for planet formation. The disks often develop a flared torus shape due to a combination of heat and radiation pressure from the central star. They can last several million years, evolving through accretion, outflows, photoevaporation, and/or condensation into larger bodies, small to large (planetesimals or planets). Though it is millions of years, this is short enough that it has been considered as a possible limiting factor in the type of planets emerging, e.g., how large a gas planet can grow, since the gas portion of the disk disappears.

The term proplyd is an abbreviation of protoplanetary disk, sometimes used generally but often specifically for some types of observed objects interpreted as protoplanetary disks: as glowing objects presumed ionized by the host star or another star and/or as shapes seen blocking light from behind. Star-forming regions typically include hot stars that produce ionizing radiation. The disks may be seen in the ultraviolet due to the ionization, or in the infrared due to thermal emission from the disk's dust. Direct imaging of such disks have been carried out by the Hubble Space Telescope, Atacama Large Millimeter Array, and Subaru Telescope.

The dust in a protoplanetary disk necessarily comes to vary in size if solid objects are forming. The dust inherited from the star-forming region is presumed to be up to micron sized. Some information about the location of different sizes can be gleaned from resolving it at different wavelengths: grains tend to emit thermal radiation most efficiently at a wavelength on the order of their diameter. Disks generally show fewer larger grains further out which matches the notion that the effects of radiation pressure on dust grains are significant.


(disk type,object type)
Further reading:
https://en.wikipedia.org/wiki/Protoplanetary_disk
https://en.wikipedia.org/wiki/Proplyd
https://dictionary.obspm.fr/index.php?formSearchTextfield=protoplanetary+disk&showAll=1
https://sites.pitt.edu/~cejones/GeoImages/0PlanetaryFormation/PlanetaryFmn/0PlanetaryFormation.html
https://public.nrao.edu/gallery/twenty-protoplanetary-disks-imaged-by-alma/
https://www.daviddarling.info/encyclopedia/P/protoplandisk.html
https://jila.colorado.edu/~pja/araa.html
https://ui.adsabs.harvard.edu/abs/2011ARA%26A..49..195A/abstract

Referenced by pages:
1.3-mm observation
AB Aurigae (AB Aur)
accretion
accretion disk
atmosphere formation
baroclinicity
barrier
Bondi radius
bouncing barrier
carbon (C)
carbon dioxide (CO2)
carbon monoxide (CO)
carbon planet
circumstellar disk
CO ladder
computational astrophysics
core accretion model
corotation resonance
cosmic dust
debris disk
direct imaging
disk
disk gap
DSHARP
dust trap
dynamical friction
dynamical instability
dynamo
electrostatic barrier
Elias 2-27
fragmentation barrier
free-floating planet (FFP)
FU Orionis star (FUor)
gas flow
giant planet
giant planet formation
giant star
grand tack hypothesis
gravitational instability (GI)
gravitational instability model
HD 163296
HD 169142
heating
HL Tau
hydrogen cyanide (HCN)
hydrogen deuteride (HD)
hydrostatic equilibrium
I band
ice
inertial wave
Infrared Space Observatory (ISO)
isolation mass
Kelvin-Helmholtz instability (KHI)
kilometer size barrier
Lindblad resonance
line tomography
MAPS
meter size barrier
millimeter astronomy
morphology
MWC 758
nebular hypothesis
Orion Disks
passive dust
PDS 70
pebble accretion
photoevaporation
planet formation
planetary embryo
planetary migration
polarimetry
protoplanetary nebula (PPN)
radial drift
radial mixing
radial-drift barrier
RODEO
Rossby wave instability (RWI)
Rossby waves
RXJ1615
snow line
solar nebula
speckle suppression
spiral density wave
stellar age determination
streaming instability
striae
T-Tauri star (TTS)
Toomre Q parameter (Q)
TW Hydrae (TW Hya)
vortensity

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