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Related Concept Videos

General External Flow Characteristics01:26

General External Flow Characteristics

481
The study of external flow is essential for creating structures and objects that interact efficiently and safely with moving fluids, such as air or water. When a body is immersed in a flowing fluid, it experiences two primary forces: drag, which opposes motion along the flow direction, and lift, which acts perpendicular to the flow. The shape, size, and orientation of the object influence these forces.Streamlined and Blunt Bodies in External FlowObjects in fluid flow are classified as...
481
Magnetostatic Boundary Conditions01:28

Magnetostatic Boundary Conditions

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An electric field suffers a discontinuity at a surface charge. Similarly, a magnetic field is discontinuous at a surface current. The perpendicular component of a magnetic field is continuous across the interface of two magnetic mediums. In contrast, its parallel component, perpendicular to the current, is discontinuous by the amount equal to the product of the vacuum permeability and the surface current. Like the scalar potential in electrostatics, the vector potential is also continuous...
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Magnetic Field Lines01:19

Magnetic Field Lines

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The representation of magnetic fields by magnetic field lines is very useful in visualizing the strength and direction of the magnetic field. Each of the magnetic field lines forms a closed loop. The field lines emerge from the north pole (N), loop around to the south pole (S), and continue through the bar magnet back to the north pole.
Magnetic field lines follow several hard-and-fast rules:
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Magnetic Field of a Solenoid01:18

Magnetic Field of a Solenoid

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A solenoid is a conducting wire coated with an insulating material, wound tightly in the form of a helical coil. The magnetic field due to a solenoid is the vector sum of the magnetic fields due to its individual turns. Therefore, for an ideal solenoid, the magnetic field within the solenoid is directly proportional to the number of turns per unit length and the current. Conversely, the magnetic field outside the solenoid is zero.
Consider a solenoid with 100 turns wrapped around a cylinder of...
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Steady, Laminar Flow Between Parallel Plates01:17

Steady, Laminar Flow Between Parallel Plates

732
Understanding steady, laminar flow between parallel plates is essential for analyzing and designing flow in narrow rectangular channels, commonly found in various water conveyance and drainage systems. The Navier-Stokes equations govern fluid motion and are generally challenging to solve due to their nonlinearity. However, simplifications are possible in certain cases, like the steady laminar flow between parallel plates. For this scenario, we assume steady, incompressible, laminar flow.
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Couette Flow01:22

Couette Flow

828
Couette flow represents the flow of fluid between two parallel plates, with one plate fixed and the other moving with a constant velocity. This configuration allows for a simplified analysis using the Navier-Stokes equations, which govern fluid motion under conditions of viscosity and incompressibility. For Couette flow, the assumptions include a steady, laminar, incompressible flow with a zero-pressure gradient in the flow direction. This flow type is beneficial for understanding shear-driven...
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Related Experiment Video

Updated: Jan 2, 2026

Experimental Investigation of Secondary Flow Structures Downstream of a Model Type IV Stent Failure in a 180° Curved Artery Test Section
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Experimental Investigation of Secondary Flow Structures Downstream of a Model Type IV Stent Failure in a 180° Curved Artery Test Section

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Highly structured slow solar wind emerging from an equatorial coronal hole.

S D Bale1,2,3,4, S T Badman5,6, J W Bonnell5

  • 1Space Sciences Laboratory, University of California, Berkeley, CA, USA. bale@berkeley.edu.

Nature
|December 6, 2019
PubMed
Summary

Scientists used the Parker Solar Probe to study the Sun's solar wind. They found evidence that low-latitude coronal holes are a key source of the slow solar wind, driven by impulsive energization mechanisms.

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Related Experiment Videos

Last Updated: Jan 2, 2026

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Area of Science:

  • Heliophysics and Space Physics
  • Solar Physics
  • Plasma Physics

Background:

  • The solar wind, a stream of plasma from the Sun, has distinct fast and slow components.
  • The origins of the slow solar wind and its heating mechanisms remain uncertain.
  • Previous observations at Earth are of a mixed and evolved solar wind, obscuring source details.

Purpose of the Study:

  • To investigate the source and characteristics of the slow solar wind closer to the Sun.
  • To identify the mechanisms responsible for solar wind heating and acceleration.

Main Methods:

  • Utilized Parker Solar Probe observations at 36 to 54 solar radii.
  • Analyzed magnetic field data, plasma flow, and Poynting flux.
  • Examined plasma-wave measurements for micro-instabilities.

Main Results:

  • Observed slow Alfvénic solar wind originating from a small equatorial coronal hole.
  • Detected intermittent magnetic field reversals associated with plasma jets and enhanced Poynting flux.
  • Identified electron and ion velocity-space micro-instabilities linked to plasma heating.

Conclusions:

  • Low-latitude coronal holes are a significant source of the slow solar wind.
  • Impulsive energization mechanisms and micro-instabilities play a crucial role in solar wind heating.