Solar rotation is able to vary with latitude because the Sun is composed of a gaseous plasma. The rate of rotation is observed to be fastest at the equator (latitude φ=0 deg), and to decrease as latitude increases. The differential rotation rate is usually described by the equation:
where ω is the angular velocity in degrees per day, φ is the solar latitude and A, B, and C are constants. The values of A, B, and C differ depending on the techniques used to make the measurement, as well as the time period studied. A current set of accepted average values is:
- A= 14.713 deg/day (± 0.0491)
- B= –2.396 deg/day (± 0.188)
- C= –1.787 deg/day (± 0.253)
Read more about Solar Rotation: Sidereal Rotation, Using Sunspots To Measure Rotation, Internal Solar Rotation
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