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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
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.
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]
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.
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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 ...
The depth of this gap depends on the temperature and viscosity of the gas and on the planet mass. In the simple scenario in which no gas crosses the gap, the migration of the planet follows the viscous evolution of the disk's gas. In the inner disk, the planet spirals inward on the viscous timescale, following the accretion of gas onto the star.
AB Aurigae b is a directly imaged protoplanet embedded within the protoplanetary disk of the young, Herbig Ae/Be star AB Aurigae. The system is about 508 light-years away: AB Aur b is located at a projected separation of about 93 AU from its host star. It may provide evidence for the formation of gas giant planets by disk instability.
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