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Related Concept Videos

Stream Function01:20

Stream Function

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In two-dimensional incompressible fluid flow, the continuity equation is essential for ensuring mass conservation, meaning that any change in fluid entering or exiting a region is balanced by a corresponding change elsewhere. For incompressible flow, where density remains constant, this requirement simplifies to the condition that the divergence of the velocity field must be zero. Mathematically, this is expressed as,
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Three-Winding Transformers01:19

Three-Winding Transformers

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Three identical single-phase transformers can be configured to form a three-phase transformer connection, which involves high-voltage and low-voltage windings. The high-voltage windings are denoted by capital letters A-B-C, while the low-voltage windings are labeled with lowercase letters a-b-c, representing their respective phases. This notation helps distinguish between the high and low voltage sides of the transformer.
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Wind Turbine Machine Models01:24

Wind Turbine Machine Models

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In the growing field of wind energy, incorporating wind turbine models into transient stability analysis is essential. Induction and synchronous machines are the primary models used, with induction machines being prevalent due to their simplicity and reliability.
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IR Frequency Region: Fingerprint Region01:03

IR Frequency Region: Fingerprint Region

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IR spectra are divided into two main regions: the diagnostic region and the fingerprint region. The diagnostic region of the spectrum lies above 1500 cm−1. The absorptions resulting from single-bond vibrations of the N–H, C–H, and O–H stretch at higher wavenumbers and appear on the left side of the spectrum. The stretching absorptions of the C≡C and C≡N occur between 2100–2300 cm−1. In contrast, those arising from stretching absorptions of the...
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Steady Flow of a Fluid Stream01:27

Steady Flow of a Fluid Stream

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Consider a control volume, such as a pipe with solid boundaries, through which fluid flows and changes direction due to the impulse exerted by the resulting force from the pipe walls. In steady flow, the mass of fluid entering the control volume at a given time, t, with velocity v1, is equal to the mass leaving after infinitesimal time dt, with velocity v2.
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The Eukaryotic Promoter Region02:40

The Eukaryotic Promoter Region

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The eukaryotic promoter region is a segment of DNA located upstream of a gene. It contains an RNA polymerase binding site, a transcription start site, and several cis-regulatory sequences.  The proximal promoter region is located in the vicinity of the gene and has cis-regulatory sequences and the core promoter. The core promoter is the binding site for RNA polymerase and is usually located between -35 and +35 nucleotides from the transcription start site. The distal promoter regions are...
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Measurements of Waves in a Wind-wave Tank Under Steady and Time-varying Wind Forcing
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Solar wind stream interaction regions throughout the heliosphere.

Ian G Richardson1,2

  • 11GPHI and Department of Astronomy, University of Maryland, College Park, MD 20742 USA.

Living Reviews in Solar Physics
|March 16, 2019
PubMed
Summary
This summary is machine-generated.

Fast solar wind streams interact with slower solar wind, forming persistent stream interaction regions. These regions influence energetic particles, cosmic rays, and Earth's geomagnetic activity.

Keywords:
Corotating interaction regionsHeliosphereHigh-speed streamsSolar wind

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Area of Science:

  • Space Physics
  • Heliophysics
  • Plasma Physics

Background:

  • The solar wind, a stream of charged particles released from the upper atmosphere of the Sun, exhibits variations in speed.
  • Fast solar wind originates from coronal holes, while slower solar wind emanates from other regions.
  • These variations lead to dynamic interactions within the heliosphere.

Purpose of the Study:

  • To review observations and discuss the formation and characteristics of stream interaction regions (SIRs).
  • To highlight the significance of SIRs in the heliosphere.
  • To explore methods for detecting and modeling SIRs.

Main Methods:

  • Review of in-situ observations from spacecraft like Helios, Pioneer, Voyager, and Ulysses.
  • Discussion of remote sensing techniques, including interplanetary scintillation and white-light imaging.
  • Overview of magnetohydrodynamic (MHD) modeling approaches.

Main Results:

  • SIRs are persistent structures formed by the interaction of fast and slow solar wind streams.
  • Observations confirm SIRs across the inner, outer, and distant heliosphere, as well as out of the ecliptic plane.
  • SIRs are significant sources of energetic particles and influence galactic cosmic ray modulation.

Conclusions:

  • Stream interaction regions are fundamental components of the heliosphere with far-reaching effects.
  • Understanding SIRs is crucial for comprehending space weather phenomena, including geomagnetic activity.
  • Advanced detection and modeling techniques are vital for studying these dynamic structures.