File:Structure of Stars (artist’s impression).jpg

Original file ‎(5,176 × 3,910 pixels, file size: 4.91 MB, MIME type: image/jpeg)

This file is from a shared repository and may be used by other projects. The description on its file description page there is shown below.

Wikipedia does not have a File page with this exact name.

Other reasons this message may be displayed:

If an image was recently created here, it may not be visible yet because of a delay in updating the database; wait a few minutes or try the purge function.
Titles on Wikipedia are case sensitive except for the first character; please check alternative capitalizations and consider adding a redirect here to the correct title.
If the page has been deleted, check the deletion log, and see Why was the page I created deleted?

File history

Click on a date/time to view the file as it appeared at that time.

	Date/Time	Thumbnail	Dimensions	User	Comment
current	16:35, 28 May 2013		5,176 × 3,910 (4.91 MB)	Stas1995	{{Information \|Description=Artist's impression of the structure of a solar-like star and a red giant. The two images are not to scale - the scale is given in the lower right corner. It is common to divide the Sun's (and solar-like stars') interior into...

The following file is a duplicate of this file (more details):

The following page uses this file:

This file contains additional information, probably added from the digital camera or scanner used to create or digitize it.

If the file has been modified from its original state, some details may not fully reflect the modified file.

Image title	Artist's impression of the structure of a solar-like star and a red giant. The two images are not to scale - the scale is given in the lower right corner. It is common to divide the Sun's (and solar-like stars') interior into three distinct zones: The uppermost is the Convective Zone. It extends downwards from the bottom of the photosphere to a depth of about 15% of the radius of the Sun. Here the energy is mainly transported upwards by (convection) streams of gas. The Radiative Zone is below the convection zone and extends downwards to the core. Here energy is transported outwards by radiation and not by convection. From the top of this zone to the bottom, the density increases 100 times. The core occupies the central region and its diameter is about 15% of that of the entire star. Here the energy is produced by fusion processes through which hydrogen nuclei are fused together to produce helium nuclei. In the Sun, the temperature is around 14 million degrees. In red giants, the convection zone is much larger, encompassing more than 35 times more mass than in the Sun.
Date and time of data generation	00:00, 6 July 2007
Source	European Southern Observatory
Credit/Provider	ESO
Short title	Structure of Stars (artist’s impression)
Keywords	Stars
Contact information	http://www.eso.org/ Karl-Schwarzschild-Strasse 2 Garching bei München, , D-85748 Germany
Usage terms	Creative Commons Attribution 3.0 Unported license