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Videos de Conceptos Relacionados

General External Flow Characteristics01:26

General External Flow Characteristics

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The study of external flow is essential for creating structures and objects that interact efficiently and safely with moving fluids, such as air or water. When a body is immersed in a flowing fluid, it experiences two primary forces: drag, which opposes motion along the flow direction, and lift, which acts perpendicular to the flow. The shape, size, and orientation of the object influence these forces.Streamlined and Blunt Bodies in External FlowObjects in fluid flow are classified as...
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Magnetostatic Boundary Conditions01:28

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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...
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Magnetic Field Lines01:19

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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.
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Magnetic Field of a Solenoid01:18

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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.
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Steady, Laminar Flow Between Parallel Plates01:17

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Understanding steady, laminar flow between parallel plates is essential for analyzing and designing flow in narrow rectangular channels, commonly found in various water conveyance and drainage systems. The Navier-Stokes equations govern fluid motion and are generally challenging to solve due to their nonlinearity. However, simplifications are possible in certain cases, like the steady laminar flow between parallel plates. For this scenario, we assume steady, incompressible, laminar flow.
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Couette Flow01:22

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Couette flow represents the flow of fluid between two parallel plates, with one plate fixed and the other moving with a constant velocity. This configuration allows for a simplified analysis using the Navier-Stokes equations, which govern fluid motion under conditions of viscosity and incompressibility. For Couette flow, the assumptions include a steady, laminar, incompressible flow with a zero-pressure gradient in the flow direction. This flow type is beneficial for understanding shear-driven...
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Video Experimental Relacionado

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Experimental Investigation of Secondary Flow Structures Downstream of a Model Type IV Stent Failure in a 180° Curved Artery Test Section
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Viento solar lento altamente estructurado que emerge de un agujero coronal ecuatorial

S D Bale1,2,3,4, S T Badman5,6, J W Bonnell5

  • 1Space Sciences Laboratory, University of California, Berkeley, CA, USA. bale@berkeley.edu.

Nature
|December 6, 2019
PubMed
Resumen

Los científicos utilizaron la sonda solar Parker para estudiar el viento solar del Sol. Encontraron evidencia de que los agujeros coronales de baja latitud son una fuente clave del viento solar lento, impulsado por mecanismos de energización impulsiva.

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Área de la Ciencia:

  • Heliofísica y Física Espacial
  • Física solar
  • Física del plasma

Sus antecedentes:

  • El viento solar, una corriente de plasma del Sol, tiene componentes rápidos y lentos distintos.
  • Los orígenes del viento solar lento y sus mecanismos de calentamiento siguen siendo inciertos.
  • Las observaciones anteriores en la Tierra son de un viento solar mezclado y evolucionado, oscureciendo los detalles de la fuente.

Objetivo del estudio:

  • Para investigar la fuente y las características del viento solar lento más cerca del Sol.
  • Identificar los mecanismos responsables del calentamiento y la aceleración del viento solar.

Principales métodos:

  • Utilizó las observaciones de la sonda solar Parker a 36 a 54 radios solares.
  • Analizaron los datos del campo magnético, el flujo de plasma y el flujo de Poynting.
  • Se han examinado las mediciones de ondas plasmáticas para detectar microinstabilidades.

Principales resultados:

  • Viento solar Alfvénico observado lento originado en un pequeño agujero coronal ecuatorial.
  • Se detectaron inversiones intermitentes del campo magnético asociadas con chorros de plasma y flujo de Poynting mejorado.
  • Microinstabilidades de velocidad de electrones e iones identificadas relacionadas con el calentamiento del plasma.

Conclusiones:

  • Los agujeros coronales de baja latitud son una fuente significativa del viento solar lento.
  • Los mecanismos de energización impulsiva y las microinstabilidades juegan un papel crucial en el calentamiento del viento solar.