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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
HH-30 (also V1213 Tauri) is an edge-on protoplanetary disk that is surrounded by jets and a disk wind. [6] HH-30 is located in the dark cloud LDN 1551 in the Taurus Molecular Cloud . The HH-30 disk is the prototype of an edge-on disk, [ 2 ] due to its early discovery with Hubble .
Only some are transitional disks between protoplanetary and debris. A few disks in this list are circumbinary disks. List of large disks This ...
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.
In January 1999, NASA announced a protoplanetary disk around HD 141569. The Hubble Space Telescope showed that the disk appears to come in two parts (inner and outer). It superficially resembles the largest gap in Saturn's rings (known as the Cassini division). The vast disk is 75 billion miles across (13 times the diameter of Neptune's orbit ...
Disk Planet Planet distance (in AU) Notes HD 100546: Disk extends out to 17: Diameter, 721 AU [1] HD 100546 b: 6.5 – GM Aurigae: 0–300 – – – Disc is warped Lynds 1551: 0.1 – – – Binary system 45 AU apart OTS 44 – – – – Second smallest brown dwarf TW Hydrae: 80: 440 [2]
Thus the formation of planetary systems is thought to be a natural result of star formation. A Sun-like star usually takes approximately 1 million years to form, with the protoplanetary disk evolving into a planetary system over the next 10–100 million years. [2] The protoplanetary disk is an accretion disk that feeds the central star. [3]
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.