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Electromagnetic Waves

Electromagnetic Waves

James Clerk Maxwell formulated a single theory combining all the electric and magnetic effects scientists knew during that time, calling the phenomena his theory predicted “Electromagnetic waves”. He brought together all the work that had been done by brilliant physicists such as Oersted, Coulomb, Gauss, and Faraday and added his own insights to develop the overarching theory of electromagnetism. Maxwell’s equations, combined with the Lorentz force law, encompass all the laws of electricity and...

Propagation of Waves

Propagation of Waves

When a wave propagates from one medium to another, part of it may get reflected in the first medium, and part of it may get transmitted to the second medium. In such a case, the interface of the two mediums can be considered as a boundary that is neither fixed nor free.
Consider a scenario where a wave propagates from a string of low linear mass density to a string of high linear mass density. In such a case, the reflected wave is out of phase with respect to the incident wave, however the...

Standing Waves

Standing Waves

Sometimes waves do not seem to move; rather, they just vibrate in place. Unmoving waves can be seen on the surface of a glass of milk kept in a refrigerator, which is one example of standing waves. Vibrations from the refrigerator motor create waves on the milk that oscillate up and down but do not seem to move across the surface. These waves are formed or created by the superposition of two or more identical moving waves in opposite directions. The waves move through each other, with their...

Electromagnetic Wave Equation

Electromagnetic Wave Equation

Maxwell's equations for electromagnetic fields are related to source charges, either static or moving. These fields act on a test charge, whose trajectory can thus be determined using suitable boundary conditions. The objective of electromagnetism is thus theoretically complete.
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Equations of Wave Motion

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Mathematically, the motion of a wave can be studied using a wavefunction. Consider a string oscillating up and down in simple harmonic motion, having a period T. The wave on the string is sinusoidal and is translated in the positive x-direction as time progresses. Sine is a function of the angle θ, oscillating between +A and −A and repeating every 2π radians. To construct a wave model, the ratio of the angle θ and the position x is considered.

Standing Waves in a Cavity

Standing Waves in a Cavity

A household microwave and lasers are examples of standing electromagnetic waves in a cavity. When two conducting metal plates are placed parallel at the nodal planes, it creates a cavity where standing waves are formed. The cavity between the two planes is analogous to a stretched string held at the points x = 0 and x = L. Here, the distance 'L' between the two planes must be an integer multiple of half of the wavelength. The wavelengths that satisfy this condition are given by:

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Related Experiment Video

Updated: Jul 12, 2026

Simulating Imaging of Large Scale Radio Arrays on the Lunar Surface

Simulating Imaging of Large Scale Radio Arrays on the Lunar Surface

Published on: July 30, 2020

Alfven waves in the solar corona.

S Tomczyk¹, S W McIntosh, S L Keil

¹High Altitude Observatory (HAO), National Center for Atmospheric Research (NCAR), Post Office Box 3000, Boulder, CO 80307-3000, USA. tomczyk@ucar.edu

Science (New York, N.Y.)

|September 1, 2007

Summary

Alfvén waves were detected in the Sun's corona, but the observed waves appear too weak to explain coronal heating. Unresolved waves might still hold the key to understanding solar coronal heating mechanisms.

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Area of Science:

Solar physics
Plasma astrophysics
Heliophysics

Background:

The Sun's corona reaches millions of degrees, a phenomenon not fully explained by current models.
Alfvén waves are proposed to transport energy from the photosphere to the corona, potentially driving this heating.
Understanding coronal heating is crucial for predicting space weather and its impact on Earth.

Purpose of the Study:

To detect and characterize Alfvén waves in the solar corona.
To assess the energy transport capability of observed Alfvén waves for coronal heating.
To investigate the role of Alfvén waves in the Sun's atmospheric energy balance.

Main Methods:

Utilized the Coronal Multi-Channel Polarimeter (CoMP) instrument at the National Solar Observatory.
Analyzed intensity, line-of-sight velocity, and linear polarization data of the solar corona.
Focused on the FeXIII 1074.7-nanometer coronal emission line.

Main Results:

Detected ubiquitous upward propagating Alfvén waves in the solar corona.
Measured wave phase speeds ranging from 1 to 4 megameters per second.
Inferred wave trajectories consistent with magnetic field direction from polarization measurements.

Conclusions:

The spatially resolved Alfvén waves detected carry insufficient energy to heat the solar corona.
The possibility remains that unresolved or smaller-scale Alfvén waves could provide the necessary energy for coronal heating.
Further investigation into unresolved wave populations is needed to fully understand coronal energy transport.