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相关概念视频

Maxwell-Boltzmann Distribution: Problem Solving01:20

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Individual molecules in a gas move in random directions, but a gas containing numerous molecules has a predictable distribution of molecular speeds, which is known as the Maxwell-Boltzmann distribution, f(v).
This distribution function f(v) is defined by saying that the expected number N (v1,v2) of particles with speeds between v1 and v2 is given by
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Radiation Pressure: Problem Solving01:09

Radiation Pressure: Problem Solving

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The radiation pressure applied by an electromagnetic wave on a perfectly absorbing surface equals the energy density of the wave. The wave's momentum also gets transferred to the surface when an electromagnetic wave is entirely absorbed by it. The rate at which momentum is transmitted to an absorbing surface perpendicular to the propagation direction equals the force on the surface.
The average value of the rate of momentum transfer divided by the absorbing area represents the average force...
366
Atomic Absorption Spectroscopy: Radiation and Light Sources01:13

Atomic Absorption Spectroscopy: Radiation and Light Sources

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Atomic absorption spectroscopy (AAS) relies on the Beer-Lambert law, which requires that the radiation source emits a narrow range of wavelengths to match the absorption characteristics of the analyte atom. The primary criteria for choosing an appropriate radiation source in AAS is to provide a precise and intense emission at specific wavelengths that will allow accurate detection of the analyte.
Two common narrow-range 'line' sources used in AAS are hollow-cathode lamps (HCLs) and...
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An object absorbing an electromagnetic wave would experience a force in the direction of propagation of the wave. This force occurs because electromagnetic waves contain and transport momentum. The force accounts for the wave's radiation pressure exerted on the object. Maxwell's prediction was confirmed in 1903 by Nichols and Hull by precisely measuring radiation pressures with a torsion balance. The measuring instrument had mirrors suspended from a fiber kept inside a glass container.
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Emission Spectra02:39

Emission Spectra

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When solids, liquids, or condensed gases are heated sufficiently, they radiate some of the excess energy as light. Photons produced in this manner have a range of energies, and thereby produce a continuous spectrum in which an unbroken series of wavelengths is present.
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The vacuum level denotes the energy threshold required for an electron to escape from a material surface. It is usually positioned above the conduction band of a semiconductor and acts as a benchmark for comparing electron energies within various materials.
Electron affinity in semiconductors refers to the energy gap between the minimum of its conduction band and the vacuum level and it is a critical parameter in determining how easily a semiconductor can accept additional electrons.
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Simulating Imaging of Large Scale Radio Arrays on the Lunar Surface
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大动态范围的恒星辐射模拟光学系统

Yu Zhang1, Yuegang Fu2,3,4, Qiang Liu5

  • 1College of Optoelectronic Engineering, Changchun University of Science and Technology, Changchun, 130022, Jilin, China. 185946585@qq.com.

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概括
此摘要是机器生成的。

这项研究引入了一种模拟恒星光谱信息的新方法,可以实现准确的色温和大动态范围模拟. 开发的光学系统可以实现高精度的光谱和大小模拟,这对于地面校准至关重要.

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科学领域:

  • 光学工程是指光学工程.
  • 天体物理学 天体物理学
  • 频谱学是一种光谱学.

背景情况:

  • 目前的恒星光谱模拟缺乏对恒星颜色温度的大动态范围模拟的能力.
  • 精确模拟恒星辐射对于高精度系统的地面校准至关重要.

研究的目的:

  • 开发一种模拟恒星光谱信息的方法,具有大动态范围和准确的色温.
  • 设计和验证用于多色温度谱和大动态范围恒星模拟的光学系统.

主要方法:

  • 提出了一种广谱,高分辨率的细分和空间光束区域调制方法.
  • 设计了一个成像和非成像恒星辐射信息模拟光学系统.
  • 集成的多色温度频谱和大动态范围的恒星模拟能力.

主要成果:

  • 实现了比±7% (450-1000nm) 更好的光谱模拟精度和3000-11,000K的颜色温度模拟精度.
  • 启用大小模拟范围为0到+12 MV,精度优于±0.05 MV.
  • 扩展了系统功能,可以在宽带和窄带模式之间切换 (半峰宽度<4.1 nm).

结论:

  • 设计的系统准确地模拟了恒星光谱信息和能量,具有很大的动态范围.
  • 该系统为高精度恒星辐射信息模拟系统的地面校准提供了理论和技术基础.
  • 扩展光谱模拟技术增强了天体物理学和光学工程中的应用.