1 / 16

The Sun: close-up of a spectral class G main sequence star

The Sun: close-up of a spectral class G main sequence star. Illustration of Kirchoff’s 1st Law. A hot object emits more radiation at all wavelengths than A cooler object (Figure 7-6). Structure of a Sunspot. Note granulation. Sunspots are regions of very strong magnetic field (2000 Gauss).

art
Download Presentation

The Sun: close-up of a spectral class G main sequence star

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript


  1. The Sun: close-up of a spectral class G main sequence star

  2. Illustration of Kirchoff’s 1st Law A hot object emits more radiation at all wavelengths than A cooler object (Figure 7-6)

  3. Structure of a Sunspot Note granulation Sunspots are regions of very strong magnetic field (2000 Gauss) Demo

  4. Sunspots represent “tubes” of magnetic field lines

  5. This causes sunspots to often occur in pairs, with opposite magnetic poles

  6. Sunspots and magnetism http://sohowww.nascom.nasa.gov/gallery/Movies/

  7. Solar magnetic fields reach far out into space

  8. The 11 Year Solar Cycle The Sun has a “heartbeat”; its properties change on a period of 11 years

  9. Latest data on this sunspot cycle

  10. The Sunspot Cycle has been going on for a long time Observations show cycle persisting, but “turning off” from 1650 to 1730 (Maunder Minimum)

  11. The Structure of the Solar Atmosphere • Photosphere • Chromosphere • Corona • Temperature increases as you go up • Outermost layer flows out into space to form the Solar Wind

  12. The solar corona

  13. The solar corona

  14. The Solar Wind • A wind past the Earth at 400 km/sec • The Sun is “melting away” • Density 19 orders of magnitude less than atmosphere • A medium for solar events • May have “sandblasted” the early atmosphere of Mars

  15. Explosions on the Sun: Solar Flares and Coronal Mass Ejections The occurrence of flares and CMEs is enhanced around The time of solar maximum

  16. The Lesson for Other Stars • Do they also have sunspots, sunspot cycles, etc? • How does all this (magnetic fields, solar wind, rotation) relate to the age of a star?

More Related