File:Solar rotation period as a function of solar latitude.png
Solar_rotation_period_as_a_function_of_solar_latitude.png (562 × 455 pixels, file size: 25 KB, MIME type: image/png)
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Summary
[edit]DescriptionSolar rotation period as a function of solar latitude.png |
English: ==Surface rotation as an equation==
The differential rotation rate is usually described by the equation: where is the angular velocity in degrees per day, is the solar latitude, A is angular velocity at the equator, and B, C are constants controlling the decrease in velocity with increasing latitude. The values of A, B, and C differ depending on the techniques used to make the measurement, as well as the time period studied.[1] A current set of accepted average values[2] is:
Plotted in python ```python import numpy as np import matplotlib.pyplot as plt
A = 14.713 B = -2.396 C = -1.787
latitude = np.linspace(0, 90, 100)
omega = A + B * np.sin(np.deg2rad(latitude))**2 + C * np.sin(np.deg2rad(latitude))**4
rotational_period = 360 / omega
plt.plot(latitude, rotational_period) plt.xlabel('Latitude (degrees)') plt.ylabel('Rotational Period (days)') plt.title('Solar rotation period') plt.grid(True) plt.show() ``` |
Date | |
Source | Own work |
Author | Cosmia Nebula |
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- ↑ Beck, J. (2000). "A comparison of differential rotation measurements". Solar Physics 191: 47–70. DOI:10.1023/A:1005226402796.
- ↑ (1990). "Rotation of Doppler features in the solar photosphere". Astrophysical Journal 351: 309–316. DOI:10.1086/168467.
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