Protoplanetary disk

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A protoplanetary disk is a rotating circumstellar disk of dense gas and dust surrounding a young newly formed star, a T Tauri star, or Herbig Ae/Be star. The protoplanetary disk may also be considered an accretion disk for the star itself, because gases or other material may be falling from the inner edge of the disk onto the surface of the star. But this process should not be confused with the accretion process thought to build up the planets themselves. Externally illuminated photo-evaporating protoplanetary disks are called proplyds.


Fraction of stars that show some evidence of having a protoplanetary disk as a function of stellar age (in millions of years). The samples are nearby young clusters and associations. Figure taken from review of Mamajek (2009).[3]

Protostars mainly form from molecular clouds consisting primarily of molecular hydrogen. When a portion of a molecular cloud reaches a critical size, mass, or density, it begins to collapse under its own gravity. As this collapsing cloud, called a solar nebula, becomes denser, random gas motions originally present in the cloud average out in favor of the direction of the nebula's net angular momentum. Conservation of angular momentum causes the rotation to increase as the nebula radius decreases. This rotation causes the cloud to flatten out—much like forming a flat pizza out of dough—and take the form of a disk. This occurs because centripetal acceleration from the orbital motion resists the gravitational pull of the star only in the radial direction, but the cloud remains free to collapse in the vertical direction. The outcome is the formation of a thin disc supported by gas pressure in the vertical direction [4]. The initial collapse takes about 100,000 years. After that time the star reaches a surface temperature similar to that of a main sequence star of the same mass and becomes visible.

It is now a T Tauri star. Accretion of gas onto the star continues for another 10 million years,[5] before the disk disappears, perhaps being blown away by the young star's solar wind, or perhaps simply ceasing to emit radiation after accretion has ended. The oldest protoplanetary disk yet discovered is 25 million years old.[6][7]

Protoplanetary Disk. Simulated Spiral Arm vs Observational Data.[8]

Protoplanetary disks around T Tauri stars differ from the disks surrounding the primary components of close binary systems with respect to their size and temperature. Protoplanetary disks have radii up to 1000 AU, and only their innermost parts reach temperatures above 1000 K. They are very often accompanied by jets.

Protoplanetary disks have been observed around several young stars in our galaxy. Recent observations by the Hubble Space Telescope have shown proplyds and planetary disks to be forming within the Orion Nebula.

Protoplanetary disks are thought to be thin structures, with a typical vertical height much smaller than the radius, and a typical mass much smaller than the central young star .[9]

The mass of a typical proto-planetary disk is dominated by its gas, however, the presence of dust grains has a major role in its evolution. Dust grains shield the mid-plane of the disk from energetic radiation from outer space that creates a dead zone in which the MRI (magnetorotational instability) no longer operates.[10][11]

It is believed that these disks consist of a turbulent envelope of plasma, also called the active zone, that encases an extensive region of quiescent gas called the dead zone.[11] The dead zone located at the mid-plane can slow down the flow of matter through the disk which prohibits achieving a steady state.

Planetary system[edit]

Protoplanetary disk surrounding the young star Elias 2-27, located some 450 light years away.[12]

The nebular hypothesis of solar system formation describes how protoplanetary disks are thought to evolve into planetary systems. Electrostatic and gravitational interactions may cause the dust and ice grains in the disk to accrete into planetesimals. This process competes against the stellar wind, which drives the gas out of the system, and gravity (accretion), which pulls material into the central T Tauri star.

Some of the moons of Jupiter, Saturn, and other planets are believed to have formed from smaller, circumplanetary analogs of the protoplanetary disks.[13][14] The formation of planets and moons in geometrically thin, gas- and dust-rich disks is the reason why the planets are arranged in an ecliptic plane. Tens of millions of years after the formation of the Solar System, the inner few AU of the Solar System likely contained dozens of moon- to Mars-sized bodies that were accreting and consolidating into the terrestrial planets that we now see. The Earth's moon likely formed after a Mars-sized protoplanet obliquely impacted the proto-Earth ~30 million years after the formation of the Solar System.

Debris disks[edit]

Artist’s impression of the water snowline around the star V883 Orionis.[15]

Gas-poor disks of circumstellar dust have been found around many nearby stars—most of which have ages in the range of ~10 million years (e.g. Beta Pictoris, 51 Ophiuchi) to billions of years (e.g. Tau Ceti). These systems are usually referred to as "debris disks". Given the older ages of these stars, and the short lifetimes of micrometer-sized dust grains around stars due to Poynting Robertson drag, collisions, and radiation pressure (typically hundreds to thousands of years), it is thought that this dust is from the collisions of planetesimals (e.g. asteroids, comets). Hence the debris disks around these examples (e.g. Vega, Alphecca, Fomalhaut, etc.) are probably not truly "protoplanetary", but represent a later stage of disk evolution where extrasolar analogs of the asteroid belt and Kuiper belt are home to dust-generating collisions between planetesimals.

Relation to abiogenesis[edit]

Based on recent computer model studies, the complex organic molecules necessary for life may have formed in the protoplanetary disk of dust grains surrounding the Sun before the formation of the Earth.[16] According to the computer studies, this same process may also occur around other stars that acquire planets.[16] (Also see Extraterrestrial organic molecules).


See also[edit]


  1. ^ Johnathan Webb (2014-11-06). "Planet formation captured in photo". BBC. 
  2. ^ "Birth of Planets Revealed in Astonishing Detail in ALMA’s ‘Best Image Ever’". NRAO. 2014-11-06. 
  3. ^ Mamajek, E.E.; Usuda, Tomonori; Tamura, Motohide; Ishii, Miki (2009). "Initial Conditions of Planet Formation: Lifetimes of Primordial Disks". AIP Conference Proceedings. 1158: 3–10. Bibcode:2009AIPC.1158....3M. arXiv:0906.5011Freely accessible. doi:10.1063/1.3215910. 
  4. ^ Pringle, J.E. (1981). "Accretion discs in astrophysics". Annual Reviews of Astronomy and Astrophysics. 19: 137–162. Bibcode:1981ARA&A..19..137P. doi:10.1146/annurev.aa.19.090181.001033. 
  5. ^ Mamajek, E.E.; Meyer, M.R.; Hinz, P.M.; Hoffmann, W.F.; Cohen, M. & Hora, J.L. (2004). "Constraining the Lifetime of Circumstellar Disks in the Terrestrial Planet Zone: A Mid-Infrared Survey of the 30 Myr old Tucana-Horologium Association". The Astrophysical Journal. 612 (1): 496–510. Bibcode:2004ApJ...612..496M. arXiv:astro-ph/0405271Freely accessible. doi:10.1086/422550. 
  6. ^ White, R.J. & Hillenbrand, L.A. (2005). "A Long-lived Accretion Disk around a Lithium-depleted Binary T Tauri Star". The Astrophysical Journal. 621 (1): L65–L68. Bibcode:2005ApJ...621L..65W. arXiv:astro-ph/0501307Freely accessible. doi:10.1086/428752. 
  7. ^ Cain, Fraser; Hartmann, Lee (3 August 2005). "Planetary Disk That Refuses to Grow Up (Interview with Lee Hartmann about the discovery)". Universe Today. Retrieved 1 June 2013. 
  8. ^ "Protoplanetary Disk: Simulated Spiral Arm vs. Observational Data". Retrieved 30 October 2015. 
  9. ^ Armitage, Philip J. (2011). "Dynamics of Protoplanetary Disks". Annual Review of Astronomy and Astrophysics. 49: 195–236. Bibcode:2011ARA&A..49..195A. arXiv:1011.1496Freely accessible. doi:10.1146/annurev-astro-081710-102521. 
  10. ^ Balbus, Steven A.; Hawley, John F. (1991). "A powerful local shear instability in weakly magnetized disks. I - Linear analysis. II - Nonlinear evolution". Astrophysical Journal. 376: 214–233. Bibcode:1991ApJ...376..214B. doi:10.1086/170270. 
  11. ^ a b Gammie, Charles (1996). "Layered Accretion In T Tauri Disks". Astrophysical Journal. 457: 355. Bibcode:1996ApJ...457..355G. doi:10.1086/176735. 
  12. ^ "Spirals with a Tale to Tell". Retrieved 6 October 2016. 
  13. ^ Canup, Robin M.; Ward, William R. (2008-12-30). Origin of Europa and the Galilean Satellites. University of Arizona Press. p. 59. ISBN 978-0-8165-2844-8. arXiv:0812.4995Freely accessible. 
  14. ^ D'Angelo, G.; Podolak, M. (2015). "Capture and Evolution of Planetesimals in Circumjovian Disks". The Astrophysical Journal. 806 (1): 29pp. Bibcode:2015ApJ...806..203D. arXiv:1504.04364Freely accessible. doi:10.1088/0004-637X/806/2/203. 
  15. ^ "Stellar Outburst Brings Water Snow Line Into View". Retrieved 15 July 2016. 
  16. ^ a b Moskowitz, Clara (29 March 2012). "Life's Building Blocks May Have Formed in Dust Around Young Sun". Retrieved 30 March 2012. 
  17. ^ "Feeding a Baby Star with a Dusty Hamburger". Retrieved 15 May 2017. 
  18. ^ "Spring Cleaning in an Infant Star System". Retrieved 3 April 2017. 
  19. ^ "Boulevard of Broken Rings". Retrieved 21 June 2016. 
  20. ^ Harrington, J.D.; Villard, Ray (24 April 2014). "RELEASE 14-114 Astronomical Forensics Uncover Planetary Disks in NASA's Hubble Archive". NASA. Archived from the original on 2014-04-25. Retrieved 2014-04-25. 

Further reading[edit]