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2MASS J04202144+2813491 (also known as Tau 042021) [3] [6] is an edge-on protoplanetary disk in the Taurus Molecular Cloud. [3]The star is hidden behind the edge-on disk. Early estimates found that it has a mass of 0.272 ±0.009 M ☉, [7] but a later study did find a higher mass of 0.3–0.4 M
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.
This study also found that the disk is surrounded by a large "foot-like" structure seen in H-alpha. [5] This "foot-like" structure could however belong to the Herbig-Haro object HH 530, which is located just north of proplyd 114-426. [7] The disk was imaged with ALMA and the disk mass was estimated to be 3.38 ±0.56 M J. [8]
Only some are transitional disks between protoplanetary and debris. A few disks in this list are circumbinary disks. List of large disks This ...
Radial drift is a process by which dust particles migrates in Protoplanetary disks during the formation of planetesimals.It involves the motion of solid particles within the gas-dominated environment surrounding a young star and is crucial to understanding the formation of planets from protoplanetary disks.
The disk wind mainly removes gas from the disk, but dust particles are also swept away from the disk. This increases the dust-to-gas ratio and promotes the formation of solid particles and subsequently the formation of planetesimals. In a typical protoplanetary disk the low mass planets migrate inwards due to gravitational interactions with the ...
The protoplanetary disk around PDS 70 was first hypothesized in 1992 [14] and fully imaged in 2006 with phase-mask coronagraph on the VLT. [2] The disk has a radius of approximately 140 au . In 2012 a large gap (~ 65 au ) in the disk was discovered, which was thought to be caused by planetary formation.
Observations suggest that gas in protoplanetary disks orbiting young stars have lifetimes of a few to several million years. [1] If planets with masses of around an Earth mass or greater form while the gas is still present, the planets can exchange angular momentum with the surrounding gas in the protoplanetary disk so that their orbits change gradually.