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A circumstellar disc (or circumstellar disk) is a torus, pancake or ring-shaped accretion disk of matter composed of gas, dust, planetesimals, asteroids, or collision fragments in orbit around a star. Around the youngest stars, they are the reservoirs of material out of which planets may form.
This is a list of circumstellar disks that have published resolved images. Many of them are protoplanetary disks or debris disks. Only some are transitional disks between protoplanetary and debris. A few disks in this list are circumbinary disks.
A circumplanetary disk will have a maximal disk size of 0.4 times the Hill radius. [8] [9] The disk also has a "dead zone" at the mid-plane that is non-turbulent and a turbulent disk surface. The dead zone is a favourable region for satellites (exomoons) to form. [10] The circumplanetary disk will go through different stages of evolution.
An accretion disk is a structure (often a circumstellar disk) formed by diffuse material [a] in orbital motion around a massive central body. The central body is most frequently a star . Friction , uneven irradiance, magnetohydrodynamic effects, and other forces induce instabilities causing orbiting material in the disk to spiral inward toward ...
A protoplanetary disk is a rotating circumstellar disc of dense gas and dust surrounding a young newly formed star, a T Tauri star, or Herbig 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.
Circumstellar disc * Circumplanetary disk; Circumstellar dust; Debris disk; Exozodiacal dust; Planetesimal; Protoplanetary disk + List of stars with proplyds; 0–9 ...
A circumsecondary disk is a disk of gas and/or dust around a star, white dwarf or substellar object that is a secondary in a star system. In rare cases the system can be aligned in a way that makes it possible for the circumsecondary disk to transit in front of the primary.
Class II objects have circumstellar disks and correspond roughly to classical T Tauri stars, while Class III stars have lost their disks and correspond approximately to weak-line T Tauri stars. An intermediate stage where disks can only be detected at longer wavelengths (e.g., at ) are known as transition-disk objects.