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Related Concept Videos

Magnetic Fields01:27

Magnetic Fields

6.0K
A moving charge or a current creates a magnetic field in the surrounding space, in addition to its electric field. The magnetic field exerts a force on any other moving charge or current that is present in the field. Like an electric field, the magnetic field is also a vector field. At any position, the direction of the magnetic field is defined as the direction in which the north pole of a compass needle points.
A magnetic field is defined by the force that a charged particle experiences...
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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 due to Moving Charges01:23

Magnetic Field due to Moving Charges

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A stationary charge creates and interacts with the electric field, while a moving charge creates a magnetic field.
Consider a point charge moving with a constant velocity. Like the electric field, the magnetic field at any point is directly proportional to the magnitude of the charge and inversely proportional to the square of the distance between the source point and the field point. However, unlike the electric field, the magnetic field is always perpendicular to the plane containing the line...
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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...
5.6K
Magnetostatic Boundary Conditions01:28

Magnetostatic Boundary Conditions

1.9K
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...
1.9K
Magnetic Damping01:17

Magnetic Damping

1.3K
Eddy currents can produce significant drag on motion, called magnetic damping. For instance, when a metallic pendulum bob swings between the poles of a strong magnet, significant drag acts on the bob as it enters and leaves the field, quickly damping the motion.
If, however, the bob is a slotted metal plate, the magnet produces a much smaller effect. When a slotted metal plate enters the field, an emf is induced by the change in flux; however, it is less effective because the slots limit the...
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Magnetic fields at the solar wind termination shock.

L F Burlaga1, N F Ness, M H Acuña

  • 1NASA/Goddard Space Flight Center, Greenbelt, Maryland 20771, USA. Leonard.F.Burlaga@nasa.gov

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|July 4, 2008
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Voyager 2 observed the complex, rippling structure of the termination shock, revealing its dynamic reformation. This finding highlights the crucial role of ionized interstellar atoms, or pickup protons, in shaping this boundary.

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Area of Science:

  • Heliophysics and Space Physics
  • Plasma Physics
  • Magnetohydrodynamics

Background:

  • Voyager 1 previously observed the transition from supersonic solar wind to subsonic heliosheath.
  • The heliospheric termination shock (TS) marks this boundary but was not directly observed by Voyager 1 due to data gaps.

Purpose of the Study:

  • To investigate the magnetic field structure and dynamics of the heliospheric termination shock.
  • To understand the nature of the TS crossing using detailed in-situ measurements.

Main Methods:

  • Analysis of magnetic field data from Voyager 2.
  • Observation period: August 31-September 1, 2007, at 83.7 astronomical units (au) from the Sun.

Main Results:

  • Voyager 2 encountered a complex, rippled, quasi-perpendicular supercritical magnetohydrodynamic shock.
  • The termination shock exhibited reformation on a timescale of a few hours, contrary to expectations of a stable boundary.
  • The observed shock structure suggests significant influence from ionized interstellar atoms (pickup protons).

Conclusions:

  • The heliospheric termination shock is a dynamic and complex structure, not a stable boundary.
  • Pickup protons play a critical role in the shock's reformation and overall structure.
  • These findings provide crucial insights into the interaction between the solar wind and the interstellar medium.