Open main menu
Home
Random
Recent changes
Special pages
Community portal
Preferences
About Wikipedia
Disclaimers
Incubator escapee wiki
Search
User menu
Talk
Dark mode
Contributions
Create account
Log in
Editing
Nebular hypothesis
(section)
Warning:
You are not logged in. Your IP address will be publicly visible if you make any edits. If you
log in
or
create an account
, your edits will be attributed to your username, along with other benefits.
Anti-spam check. Do
not
fill this in!
== Meaning of ''accretion'' == Use of the term "[[accretion disk]]" for the [[protoplanetary disk]] leads to confusion over the [[planetary accretion]] process. The protoplanetary disk is sometimes referred to as an accretion disk, because while the young [[T Tauri star|T Tauri]]-like protostar is still contracting, gaseous material may still be falling onto it, accreting on its surface from the disk's inner edge.<ref name=Yorke1999 /> In an accretion disk, there is a net flux of mass from larger radii toward smaller radii.<ref name=lynden-bell_1974 /> However, that meaning should not be confused with the process of accretion forming the planets. In this context, accretion refers to the process of cooled, solidified grains of dust and ice orbiting the [[protostar]] in the protoplanetary disk, colliding and sticking together and gradually growing, up to and including the high-energy collisions between sizable [[planetesimal]]s.<ref name=Kokubo2002 /> In addition, the [[giant planet]]s probably had accretion disks of their own, in the first meaning of the word.<ref name=dangelo_podolak_2015>{{cite journal |last=D'Angelo |first=G. |author2= Podolak, M. |title= Capture and Evolution of Planetesimals in Circumjovian Disks |journal= The Astrophysical Journal |date= 2015 |volume=806 |issue=1 |pages=29pp |doi= 10.1088/0004-637X/806/2/203|arxiv = 1504.04364 |bibcode = 2015ApJ...806..203D|s2cid=119216797 }}</ref> The clouds of captured hydrogen and helium gas contracted, spun up, flattened, and deposited gas onto the surface of each giant [[protoplanet]], while solid bodies within that disk accreted into the giant planet's regular moons.<ref name=Canup2002>{{cite journal |last=Canup |first=Robin M. |author1-link=Robin Canup |author2= Ward, William R. |title= Formation of the Galilean Satellites: Conditions of Accretion |journal= The Astronomical Journal |date=2002 |volume=124 |issue=6 |pages=3404β3423 |doi= 10.1086/344684 |url= http://www.boulder.swri.edu/~robin/cw02final.pdf |bibcode= 2002AJ....124.3404C|s2cid=47631608 }}</ref>
Edit summary
(Briefly describe your changes)
By publishing changes, you agree to the
Terms of Use
, and you irrevocably agree to release your contribution under the
CC BY-SA 4.0 License
and the
GFDL
. You agree that a hyperlink or URL is sufficient attribution under the Creative Commons license.
Cancel
Editing help
(opens in new window)