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Related Concept Videos

Magnetic Field Lines01:19

Magnetic Field Lines

4.1K
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:
4.1K
Magnetic Field of a Solenoid01:18

Magnetic Field of a Solenoid

3.8K
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...
3.8K
Magnetic Field due to Moving Charges01:23

Magnetic Field due to Moving Charges

8.5K
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...
8.5K
Magnetic Field Of A Current Loop01:16

Magnetic Field Of A Current Loop

4.4K
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.
4.4K
Magnetic Vector Potential01:15

Magnetic Vector Potential

573
In electrostatics, the electric field can be written as the negative gradient of the potential. In magnetostatics, the zero divergence of the magnetic field ensures that the magnetic field can be expressed as the curl of a vector potential. This potential is known as the magnetic vector potential.
Consider an ideal solenoid with n turns per unit length and radius R. If I is the current through the solenoid, the magnetic field inside the solenoid is expressed as the product of vacuum...
573
Magnetic Field Due To A Thin Straight Wire01:28

Magnetic Field Due To A Thin Straight Wire

4.8K
Consider an infinitely long straight wire carrying a current I. The magnetic field at point P at a distance a from the origin can be calculated using the Biot-Savart law.
4.8K

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Mapping the Sun's coronal magnetic field using the Zeeman effect.

Thomas A Schad1, Gordon J D Petrie2, Jeffrey R Kuhn3

  • 1National Solar Observatory, 22 'Ōhi'a Kū Street, Makawao, HI 96768, USA.

Science Advances
|September 11, 2024
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Summary
This summary is machine-generated.

Scientists created new maps of the Sun's magnetic field in the corona using advanced coronagraphy. These unprecedented measurements offer crucial insights into solar wind, coronal heating, and space weather forecasting.

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Area of Science:

  • * Solar Physics
  • * Astrophysics
  • * Space Weather

Background:

  • * Remote sensing of the solar coronal magnetic field is limited, hindering research into coronal heating, solar wind generation, and energy release events.
  • * Understanding the Sun's magnetic field is crucial for predicting solar flares and eruptive phenomena.

Purpose of the Study:

  • * To develop and demonstrate a novel method for mapping the magnetic field in the solar corona.
  • * To provide observational constraints for magnetohydrodynamic (MHD) models of the solar corona.
  • * To improve space weather research and forecasting.

Main Methods:

  • * Utilized advancements in large aperture solar coronagraphy.
  • * Measured polarized spectra emitted at 1074 nm by Fe+12 ions in the active corona.
  • * Detected Zeeman effect signatures indicative of the coronal magnetic field.

Main Results:

  • * Generated unprecedented maps of polarized spectra from the active solar corona.
  • * Identified clear signatures of the Zeeman effect, directly correlating with the coronal magnetic field.
  • * Provided valuable observational data for validating and constraining global MHD models.

Conclusions:

  • * The new technique offers a powerful tool for remote sensing of the coronal magnetic field.
  • * These measurements significantly advance our ability to study coronal heating and solar wind.
  • * Improved coronal modeling based on these findings will enhance space weather forecasting capabilities.