Assignment (Coronal Holes and High Speed Streams)
Contact Yaireska.M.ColladoVega@nasa.gov or jenna.l.zink@nasa.gov if you have any questions pertaining to this assessment.
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1. Why is there solar wind?
2. Does slow solar wind generally originate from high or low latitudes on the Sun?
3. What is the typical speed for the slow solar wind?
4. What is the typical density for the slow solar wind?
5. Does fast solar wind generally originate from high or low latitudes on the Sun?
6. What is the typical speed for fast solar wind?
7. What is the typical density for fast solar wind?
8. What is a coronal hole? How does the plasma density of a coronal hole compare to the rest of the corona?
9. Where are the coronal holes typically found during solar minimum, and how does that change at solar maximum?
11. What is a high speed stream, and how is it related to a coronal hole?
12. What is a corotating interaction region (CIR) and stream interaction region (SIR)?
13. How does a geomagnetic storm caused by a high speed stream differ from one caused by a CME?
14. How are high speed streams related to energetic electron fluxes in the magnetosphere?
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