The solar system rotation
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The Solar System Rotation
Planetary Rotation Rates
The planets in our solar system exhibit a wide range of rotation periods, with no clear correlation between their size, distance from the Sun, and rotation speed. For instance, Jupiter, the largest planet, completes a rotation in less than ten hours, while Mars, a much smaller planet, takes over twenty-four hours to rotate1. The rotation periods of the seven principal planets are as follows: Mercury (24 hours 5 minutes 28 seconds), Venus (23 hours 21 minutes 21 seconds), Earth (23 hours 56 minutes 4 seconds), Mars (24 hours 37 minutes 22 seconds), Jupiter (9 hours 55 minutes 26 seconds), Saturn (10 hours 29 minutes 17 seconds), and Uranus (9 hours 30 minutes, approximately)1.
Solar Rotation
The Sun, the central star of our solar system, also rotates on its axis, with a rotation period of approximately 607 hours and 48 minutes1. Observations of solar rotation have been conducted using two primary methods: tracking the positions of surface tracers and measuring line-of-sight velocities through the Doppler effect3. These methods have revealed that the Sun does not rotate uniformly; the core rotates significantly faster than the surface, with the core's rotation rate being 2 to 9 times that of the surface4 7.
Differential Rotation in the Sun
The Sun's rotation is characterized by differential rotation, where different parts of the Sun rotate at different rates. The radiative interior of the Sun rotates roughly uniformly, while the convection zone exhibits a more complex rotation pattern, with layers of rotational shear at the base of the convection zone and near the surface6 10. This differential rotation is influenced by various factors, including the Coriolis force and the structure of the convective layer9.
Rotation of Solid Bodies in the Solar System
The rotation of solid bodies in the solar system, such as planets and moons, can be influenced by several factors, including elastic distortion, nonprincipal axis rotation, precessing orbits, and internal dissipation2. These factors can be analyzed using Hamiltonian theory, which helps in understanding phenomena like the Chandler wobble and spin-orbit coupling2. Observational methods such as laser ranging and Very Long Baseline Interferometry have been used to determine the rotation of Earth and the Moon with high accuracy5.
Conclusion
The rotation of the solar system's bodies, from planets to the Sun, presents a complex and varied picture. While planets exhibit a wide range of rotation periods with no clear pattern, the Sun's rotation is characterized by significant differential rotation, with the core rotating much faster than the surface. Understanding these rotational dynamics involves a combination of observational techniques and theoretical models, providing insights into the intricate workings of our solar system.
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Rotation of the Planets
The rotation of the planets is like an eclipse to a savage, an event which he knows occurs but of the cause of which he is ignorant.
Rotation of solid bodies in the solar system
The Hamiltonian theory developed here can easily analyze the rotation of solid solar system bodies in the gravitational field of an exterior body, with applications in the Chandler wobble, moon wobble, spin-orbit coupling, and tidal evolution.
The rotation of the Sun
The rotation of the Sun can be determined using two methods: measuring daily or monthly positions of tracers on the surface or in the corona, and measuring line-of-sight velocities in spectrum lines.
Rapid rotation of the solar interior
The Sun's core rotates 2-9 times as rapidly as its surface, demonstrating a nonuniform rotation and rapid internal rotation.
Highly CitedRotation of the Solar System Bodies
Solar System bodies rotate, with different methods determining their rotation accuracy, depending on their size, shape, and structure.
Solar Interior Rotation and its Variation
The solar interior rotation has been determined through continuous helioseismic observations, revealing core and radiative interior rotation, tachocline shear layer, differential rotation, near-surface shear, and torsional oscillation.
Highly CitedFrom solar-like to antisolar differential rotation in cool stars
Cool stars with large Rossby numbers can sustain anti-solar differential rotation, governed by the Coriolis force in the force balance.
Highly CitedThe Internal Rotation of the Sun
Helioseismology has revolutionized our understanding of the Sun's internal rotation, revealing a roughly uniform rotation and a different rate dependence than previously expected.
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