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Related Concept Videos

Gyroscope: Precession01:24

Gyroscope: Precession

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Precession can be demonstrated effectively through a spinning top. If a spinning top is placed on a flat surface near the surface of the Earth at a vertical angle and is not spinning, it will fall over due to the force of gravity producing a torque acting on its center of mass. However, if the top is spinning on its axis, it precesses about the vertical direction, rather than topple over due to this torque. Precessional motion is a combination of a steady circular motion of the axis and the...
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Apparent Weight and the Earth's Rotation01:28

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Since all objects on the Earth's surface move through a circle every 24 hours, there must be a net centripetal force on each object, directed towards the center of that circle. The points of the north and south poles are the only exception to this rule.
For an object on the Earth's equator, the net centripetal force that accounts for its rotation is the Earth's pull towards its center, or the weight minus the normal force that prevents it from piercing into the Earth's surface....
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Reduced Mass Coordinates: Isolated Two-body Problem01:12

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In classical mechanics, the two-body problem is one of the fundamental problems describing the motion of two interacting bodies under gravity or any other central force. When considering the motion of two bodies, one of the most important concepts is the reduced mass coordinates, a quantity that allows the two-body problem to be solved like a single-body problem. In these circumstances, it is assumed that a single body with reduced mass revolves around another body fixed in a position with an...
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Rotation of Asymmetric Top01:11

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By definition, a spherically symmetric body has the same moment of inertia about any axis passing through its center of mass. This situation changes if there is no spherical symmetry. Since most rigid bodies are not spherically symmetric, these require special treatment.
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Tidal Forces01:06

Tidal Forces

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The origin of Earth's ocean tides has been a subject of continuous investigation for over 2000 years. However, the work of Newton is considered to be the beginning of the proper understanding of the phenomenon. Ocean tides are the result of gravitational tidal forces. These same tidal forces are present in any astronomical body; they are responsible for the internal heat that creates the volcanic activity on Io, one of Jupiter's moons, and the breakup of stars that get too close to...
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Conservation of Angular Momentum: Application01:18

Conservation of Angular Momentum: Application

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A system's total angular momentum remains constant if the net external torque acting on the system is zero. Examples of such systems include a freely spinning bicycle tire that slows over time due to torque arising from friction, or the slowing of Earth's rotation over millions of years due to frictional forces exerted on tidal deformations. However in the absence of a net external torque, the angular momentum remains conserved. The conservation of angular momentum principle requires a...
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Magnetically Induced Rotating Rayleigh-Taylor Instability
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Flare differentially rotates sunspot on Sun's surface.

Chang Liu1,2,3, Yan Xu1,2,3, Wenda Cao2,3

  • 1Space Weather Research Laboratory, New Jersey Institute of Technology, University Heights, Newark, New Jersey 07102-1982, USA.

Nature Communications
|October 11, 2016
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Solar flares can unexpectedly cause sunspots to rotate. This study observed non-uniform sunspot rotation linked to flare activity, challenging previous assumptions about solar dynamics.

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Area of Science:

  • Solar Physics
  • Plasma Astrophysics
  • Heliophysics

Background:

  • Sunspots are magnetic field concentrations on the solar photosphere.
  • Solar flares, originating in the corona, were not thought to directly perturb the dense photosphere with bulk motion.
  • Previous models did not account for direct photospheric responses to coronal magnetic reconnection.

Purpose of the Study:

  • To investigate the potential for solar flares to induce direct physical changes in sunspots.
  • To analyze the relationship between solar flare events and sunspot dynamics.
  • To challenge the established understanding of energy and momentum transfer during solar flares.

Main Methods:

  • Utilized the high-resolution 1.6-meter New Solar Telescope for detailed observations.
  • Supplemented solar telescope data with magnetic field data from the Solar Dynamics Observatory.
  • Analyzed the spatiotemporal characteristics of sunspot rotation during a solar flare event.

Main Results:

  • Observed sudden, flare-induced rotation of a sunspot.
  • Demonstrated non-uniform rotation across the sunspot, with varying acceleration rates.
  • Correlated rotational acceleration with peaks in hard X-ray emission from the flare ribbon.

Conclusions:

  • Solar flares can directly perturb the solar photosphere, causing sunspot rotation.
  • The observed rotation is likely driven by changes in the surface Lorentz force due to coronal restructuring.
  • Findings impact our understanding of energy and momentum transport in solar flare phenomena.