the sun…a star in our solar system (continued)

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The Sun…a star in our solar system (continued)

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The Sun…a star in our solar system (continued). But first…see a solar twin tonight. Beta Canum Venaticorum…look almost up and a little east at 9PM. Beta Canum Venaticorum (Beta CVn). Spectral type: G0V Temperature: 5930 K Luminosity (relative to Sun): 1.12 Distance: 27.3 light years - PowerPoint PPT Presentation

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Page 1: The Sun…a star in our solar system (continued)

The Sun…a star in our solar system (continued)

Page 2: The Sun…a star in our solar system (continued)

But first…see a solar twin tonight

Beta Canum Venaticorum…look

almost up and a little east at 9PM

Page 3: The Sun…a star in our solar system (continued)

Beta Canum Venaticorum (Beta CVn)

• Spectral type: G0V• Temperature: 5930 K• Luminosity (relative to

Sun): 1.12• Distance: 27.3 light

years• Judged best

candidate by astronomer Margaret Turnbull to try and communicate with them

Page 4: The Sun…a star in our solar system (continued)

Next topic: solar activity

The Sun doesn’t always look like it does today

Page 5: The Sun…a star in our solar system (continued)

Sunspots illustrate the rotation of the Sun

Sunspots over several days

The Sun rotates with a period of 27 days (a good indicator of its age)

Page 6: The Sun…a star in our solar system (continued)

Closeup of a sunspot

Sunspots are regions of strong magnetics fields (0.2 -0.4 Tesla)

Page 7: The Sun…a star in our solar system (continued)

Sunspots and their strong magnetic fields are related to more mysterious aspects of

the Sun

Above the photosphere are more rarefied and hotter parts of the solar atmosphere

Page 8: The Sun…a star in our solar system (continued)

The Chromosphere-region above the photosphere, and substantially hotter

Page 9: The Sun…a star in our solar system (continued)

The Solar Corona

What is it? How did it get that way?

Page 10: The Sun…a star in our solar system (continued)

The X-Ray Sun

Page 11: The Sun…a star in our solar system (continued)

The Temperature Profile in the Solar Atmosphere

Page 12: The Sun…a star in our solar system (continued)

The process or processes responsible for heating the solar corona almost certainly

involve the solar magnetic field

We just don’t know how

Page 13: The Sun…a star in our solar system (continued)

The hot, rarefield, magnetically-dominated parts of the solar atmosphere show continual activity and energy release

erupting solar prominence...April 21, 2010

Page 14: The Sun…a star in our solar system (continued)

Solar activity includes two violent types of events

• Solar flares

• Coronal mass ejections

Page 15: The Sun…a star in our solar system (continued)

Coronal mass ejections

A loop of matter “blasts off” from the Sun

Page 16: The Sun…a star in our solar system (continued)

Solar flare…the movie

The solar flare of April 21, 2002, shown on Astronomy Picture of Day for November 6,

2007

Page 17: The Sun…a star in our solar system (continued)

Why are flares and coronal mass ejections important?

• They are dangerous! They can generate levels of radiation in interplanetary space that are lethal

• They are part of, and play a role in, the development of the solar wind

Page 18: The Sun…a star in our solar system (continued)

Sunspots and solar activity: they come and go

Sept. 21, 2000 Jan. 26, 2008

Page 19: The Sun…a star in our solar system (continued)

The 11 year solar cycle: where are we now?

Page 20: The Sun…a star in our solar system (continued)

The 11 year solar cycle goes back to the time of Galileo

Maunder Minimum