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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 ...
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.
First protoplanetary disc around a pulsar discovered 4U 0142+61: 2006 Brightest star with a protoplanetary disc Vega: 2005 Not confirmed See also.
Possible processes that cause the migration include orbital friction while the protoplanetary disk is still full of hydrogen and helium gas [38] and exchange of angular momentum between giant planets and the particles in the protoplanetary disc. [39] [40] [41] One other problem is the detailed features of the planets.
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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