Description
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 shown.
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)
Variables
ω |
angular velocity (°/day) |
A |
constant – current set of accepted average values : 14.713 deg/day (± 0.0491) (°/day) |
B |
constant – current set of accepted average values : -2.396 deg/day (± 0.188) (°/day) |
ϕ |
solar latitude (degree) |
C |
constant – current set of accepted average values : -1.787 deg/day (± 0.253) (°/day) |
FREQUENTLY ASKED QUESTIONS
The rate of solar rotation decreases as latitude increases. The equator has the fastest rotation rate, and the rotation rate slows down as you move towards the poles.
The differential rotation rate of the Sun is usually described by the equation ω = A – B sin^2(φ) – C sin^4(φ), where ω is the angular velocity, φ is the latitude, and A, B, and C are constants.
The accepted average values for the constants A, B, and C in the solar rotation equation are A = 14.713 deg/day ± 0.0491, B = 2.396 deg/day ± 0.188, and C = 1.787 deg/day ± 0.253.
The angular velocity of the Sun, ω, decreases as latitude increases. At the equator, the angular velocity is maximum, and it decreases as you move towards the poles.
Understanding solar rotation is crucial in the context of astrophysics as it helps us understand the internal dynamics of the Sun, its magnetic field, and its impact on the solar system. It also provides insights into the formation and evolution of stars.
