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Electromagnetic Waves01:30

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 Waves01:07

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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 Waves01:17

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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 Equation01:24

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Equations of Wave Motion01:02

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Standing Waves in a Cavity01:28

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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Simulating Imaging of Large Scale Radio Arrays on the Lunar Surface
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Published on: July 30, 2020

Alfven las ondas en la corona solar.

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
PubMed
Resumen

Se detectaron ondas de Alfvén en la corona del Sol, pero las ondas observadas parecen demasiado débiles para explicar el calentamiento coronal. Las ondas no resueltas aún podrían ser la clave para comprender los mecanismos de calentamiento de la corona solar.

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Área de la Ciencia:

  • Física solar Física solar es la física de la energía solar.
  • La astrofísica del plasma es la astrofísica del plasma.
  • Heliofísica es la heliofísica.

Sus antecedentes:

  • La corona del Sol alcanza millones de grados, un fenómeno que no se explica completamente por los modelos actuales.
  • Se propone que las ondas de Alfvén transporten energía de la fotosfera a la corona, potencialmente impulsando este calentamiento.
  • Comprender el calentamiento coronal es crucial para predecir el clima espacial y su impacto en la Tierra.

Objetivo del estudio:

  • Para detectar y caracterizar las ondas de Alfvén en la corona solar.
  • Evaluar la capacidad de transporte de energía de las ondas de Alfvén observadas para el calentamiento coronal.
  • Para investigar el papel de las ondas de Alfvén en el equilibrio de energía atmosférica del Sol.

Principales métodos:

  • Utilizó el instrumento Polarímetro Coronal Multicanal (CoMP) en el Observatorio Solar Nacional.
  • Se analizaron la intensidad, la velocidad de la línea de visión y los datos de polarización lineal de la corona solar.
  • Centrado en la línea de emisión coronal FeXIII 1074.7-nanómetro.

Principales resultados:

  • Se han detectado ondas de Alfvén ubicuas que se propagan hacia arriba en la corona solar.
  • Las velocidades de fase de onda medidas oscilan entre 1 y 4 megametros por segundo.
  • Las trayectorias de ondas inferidas son consistentes con la dirección del campo magnético a partir de las mediciones de polarización.

Conclusiones:

  • Las ondas de Alfvén detectadas con resolución espacial llevan una energía insuficiente para calentar la corona solar.
  • Queda la posibilidad de que las ondas de Alfvén no resueltas o de menor escala puedan proporcionar la energía necesaria para el calentamiento coronal.
  • Se necesitan más investigaciones sobre las poblaciones de ondas no resueltas para comprender completamente el transporte de energía coronal.