Jump to content
Main menu
Main menu
move to sidebar
hide
Navigation
Main page
Recent changes
Random page
Help about MediaWiki
Special pages
Niidae Wiki
Search
Search
Appearance
Create account
Log in
Personal tools
Create account
Log in
Pages for logged out editors
learn more
Contributions
Talk
Editing
Sun
(section)
Page
Discussion
English
Read
Edit
View history
Tools
Tools
move to sidebar
hide
Actions
Read
Edit
View history
General
What links here
Related changes
Page information
Appearance
move to sidebar
hide
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!
=== Convective zone === {{Main|Convection zone}} The Sun's convection zone extends from 0.7 solar radii (500,000 km) to near the surface. In this layer, the solar plasma is not dense or hot enough to transfer the heat energy of the interior outward via radiation. Instead, the density of the plasma is low enough to allow convective currents to develop and move the Sun's energy outward towards its surface. Material heated at the tachocline picks up heat and expands, thereby reducing its density and allowing it to rise. As a result, an orderly motion of the mass develops into thermal cells that carry most of the heat outward to the Sun's photosphere above. Once the material diffusively and radiatively cools just beneath the photospheric surface, its density increases, and it sinks to the base of the convection zone, where it again picks up heat from the top of the radiative zone and the convective cycle continues. At the photosphere, the temperature has dropped 350-fold to {{convert|5,700|K|F}} and the density to only 0.2 g/m<sup>3</sup> (about 1/10,000 the density of air at sea level, and 1 millionth that of the inner layer of the convective zone).<ref name=NASA1 /> The thermal columns of the convection zone form an imprint on the surface of the Sun giving it a granular appearance called the [[solar granulation]] at the smallest scale and [[supergranulation]] at larger scales. Turbulent convection in this outer part of the solar interior sustains "small-scale" dynamo action over the near-surface volume of the Sun.<ref name=NASA1 /> The Sun's thermal columns are [[Bénard cells]] and take the shape of roughly hexagonal prisms.<ref>{{Cite book |last=Mullan |first=D. J. |title=From the Sun to the Great Attractor |year=2000 |publisher=[[Springer Science+Business Media|Springer]] |isbn=978-3-540-41064-5 |editor-last=Page |editor-first=D. |page=22 |chapter=Solar Physics: From the Deep Interior to the Hot Corona |access-date=22 August 2020 |editor-last2=Hirsch |editor-first2=J. G. |chapter-url=https://books.google.com/books?id=rk5fxs55_OkC&pg=PA22 |archive-url=https://web.archive.org/web/20210417080656/https://books.google.com/books?id=rk5fxs55_OkC&pg=PA22 |archive-date=17 April 2021 |url-status=live}}</ref>
Summary:
Please note that all contributions to Niidae Wiki may be edited, altered, or removed by other contributors. If you do not want your writing to be edited mercilessly, then do not submit it here.
You are also promising us that you wrote this yourself, or copied it from a public domain or similar free resource (see
Encyclopedia:Copyrights
for details).
Do not submit copyrighted work without permission!
Cancel
Editing help
(opens in new window)
Search
Search
Editing
Sun
(section)
Add topic