The Sun as We See It Lecture 9

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Presentation transcript:

The Sun as We See It Lecture 9

Further properties of the Sun The chemical composition of the Sun: cosmic composition The luminosity of the Sun = 3.85E+26 Watts The age of the Sun (how could we know this?) Comparison of other objects (M4, Arcturus)

The Sun Today

Sunspots can be more numerous and larger Sun of October 30, 2003

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

Solar magnetic fields reach far out into space

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

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

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

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

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?

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