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Related Concept Videos

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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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 Flux01:18

Magnetic Flux

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The magnetic flux measures the number of magnetic field lines passing through a given surface area. The SI unit for magnetic flux is the weber (Wb). Magnetic flux is a scalar quantity. It depends on three factors: the strength of the magnetic field B, the area through which the field lines pass, and the relative orientation of the field with the surface area.
Suppose a surface is divided into elements of area dA. For each element, the component of the magnetic field that is normal to the...
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Magnetism01:30

Magnetism

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Magnets are commonly found in everyday objects, such as toys, hangers, elevators, doorbells, and computer devices. Experimentation on these magnets shows that all magnets have two poles: one is labeled north (N) and the other south (S). Magnetic poles repel if they are alike and attract if unlike. Moreover, both poles of a magnet attract unmagnetized pieces of iron.
An individual magnetic pole cannot be isolated. No matter how small, every piece of a magnet contains a north pole and a south...
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Magnetic Field Of A Current Loop01:16

Magnetic Field Of A Current Loop

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Consider a circular loop with a radius a, that carries a current I. The magnetic field due to the current at an arbitrary point P along the axis of the loop can be calculated using the Biot-Savart law.
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Energy In A Magnetic Field01:24

Energy In A Magnetic Field

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If a magnetic field is sustained, there must be a current in a closed circuit or loop, implying some energy has been spent in creating the field. If this energy is not dissipated via the circuit's resistance, it is stored in the field.
Take an ideal inductor with zero resistance. Although it's practically impossible, assume that the coil's resistance is so small that it is practically negligible. The loss of the field's energy to dissipate thermal energy (or heat) is thus...
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Using Neutron Spin Echo Resolved Grazing Incidence Scattering to Investigate Organic Solar Cell Materials
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Parker Solar Probe Enters the Magnetically Dominated Solar Corona.

J C Kasper1, K G Klein2, E Lichko2

  • 1BWX Technologies, Inc., Washington, DC 20001, USA and Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, Michigan 48109, USA.

Physical Review Letters
|January 14, 2022
PubMed
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Parker Solar Probe sampled solar wind plasma below the Sun's Alfvén critical surface. Magnetic pressure dominated, suggesting suppressed reconnection within a pseudostreamer region.

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Area of Science:

  • * Solar Physics
  • * Plasma Physics
  • * Astrophysics

Background:

  • * The solar corona's high temperatures and magnetic fields generate solar wind streams expanding into space.
  • * Understanding the solar wind's origin and properties near the Sun is crucial for space weather prediction.
  • * Parker Solar Probe's mission is to explore the Sun's atmosphere and solar wind.

Purpose of the Study:

  • * To report the spectrum of turbulence in the solar wind below the Alfvén critical surface.
  • * To analyze the plasma conditions and magnetic field characteristics within 13 million km of the Sun.
  • * To investigate the nature of the solar wind flow and its relationship to coronal magnetic structures.

Main Methods:

  • * In-situ measurements by Parker Solar Probe.
  • * Analysis of plasma properties including Alfvén Mach number and pressure dominance (magnetic, ion, electron).
  • * Magnetic mapping to infer coronal magnetic field line expansion and pseudostreamer identification.

Main Results:

  • * Parker Solar Probe crossed below the Alfvén critical surface, sampling sub-Alfvénic plasma (Mach number 0.79).
  • * Magnetic pressure dominated both ion and electron pressure in the sampled region.
  • * Turbulence spectrum below the Alfvén critical surface was characterized.
  • * Magnetic mapping indicated a steady flow emerging from rapidly expanding coronal magnetic field lines above a pseudostreamer.

Conclusions:

  • * The sub-Alfvénic nature of the solar wind flow may result from suppressed magnetic reconnection at the pseudostreamer base.
  • * Unusually low plasma densities in the region support the hypothesis of suppressed reconnection.
  • * The findings provide insights into the dynamics of the solar wind close to the Sun.