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Atomic Emission Spectroscopy: Overview01:20

Atomic Emission Spectroscopy: Overview

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Atomic emission spectroscopy (AES) is an analytical technique used to determine the elemental composition of a sample by analyzing the light emitted from excited atoms. In AES, atoms in a sample are excited to higher energy levels by thermal energy from high-temperature sources, such as plasma, arcs, or sparks. When these excited atoms return to lower energy states, they emit light at specific wavelengths characteristic of each element. The resulting atomic emission spectrum, which consists of...
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Atomic Emission Spectroscopy: Interference01:30

Atomic Emission Spectroscopy: Interference

555
In atomic emission spectroscopy (AES), high-temperature atomizers excite a broad range of elements and molecules that generate complex emissions from sources such as oxides, hydroxides, and flame combustion products in the flame or plasma. Several strategies can be employed to minimize spectral interferences caused by overlapping emission lines or bands. These include increasing instrument resolution, choosing alternative emission lines, optimally placing the detector in low-background regions,...
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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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Atomic Spectroscopy: Effects of Temperature01:27

Atomic Spectroscopy: Effects of Temperature

804
Atomization, converting samples into gas-phase atoms and ions, is essential for atomic spectroscopy. The flame temperature required for atomization affects the efficiency of the atomic spectroscopic methods by increasing the atomization efficiency and the relative population of the excited and ground states.
At thermal equilibrium, the relative populations of excited and ground state atoms can be estimated using the Maxwell–Boltzmann distribution. For example, an increase in temperature...
804
Atomic Emission Spectroscopy: Lab01:29

Atomic Emission Spectroscopy: Lab

507
AES is a powerful analytical technique, especially effective when used with plasma sources, producing abundant spectra in characteristic emission lines. The Inductively Coupled Plasma (ICP), in particular, yields superior quantitative analytical data due to its high stability, low noise, low background, and minimal interferences under optimal experimental conditions. However, newer air-operated microwave sources are emerging as promising alternatives that could be more cost-effective than...
507
Atomic Nuclei: Larmor Precession Frequency01:11

Atomic Nuclei: Larmor Precession Frequency

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The earth's gravitational field produces a 'twisting force' perpendicular to the angular momentum of a spinning mass (such as a spinning top) that causes the mass to 'wobble' around the gravitational field axis in a phenomenon called precession. Similarly, the magnetic moment (μ) of a spinning nucleus precesses due to an external magnetic field directed along the z-axis. The precession of the magnetic moment vector about the magnetic field is called Larmor precession,...
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Applying X-ray Imaging Crystal Spectroscopy for Use as a High Temperature Plasma Diagnostic
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F-コロナ減少とK-コロナ微細構造の近日観測

R A Howard1, A Vourlidas2, V Bothmer3

  • 1US Naval Research Laboratory, Washington, DC, USA. Russ.Howard@nrl.navy.mil.

Nature
|December 6, 2019
PubMed
まとめ
この要約は機械生成です。

新しいパーカー・ソーラー・プローブの観測は,太陽の近くの塵のないゾーンと,磁気流のロープや島を含む小さな太陽噴火の詳細なプラズマ構造を明らかにしています. これは太陽のコロナ動態と進化の洞察を与えてくれます

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科学分野:

  • 太陽物理学
  • プラズマ物理学
  • 宇宙科学

背景:

  • 太陽のコロナ (K-コロナとF-コロナ) の遠隔観測は距離によって制限されている.
  • 以前の研究では 理論的に予測された太陽の近くの 塵のないゾーンが確認できませんでした
  • 構造と小さな太陽のイベントの開始は不確実です.

研究 の 目的:

  • パーカー・ソーラー・プローブを使用して,かつてないほど近い距離 (0.16-0.25 AU) で太陽のコロナをイメージする.
  • 太陽の近くにある 塵のない領域の 存在を調査するためです
  • 小さな太陽噴火の 微細なプラズマ構造を解明するためです

主な方法:

  • パーカー・ソーラー・プローブの近日点を通過する時の太陽の冠を画像化している.
  • 粉塵の分布を推測するために,短い延長でF-冠の強さを分析する.
  • 太陽噴火の微細なプラズマ構造を解明する.

主要な成果:

  • 短い延長でF-冠の強度の減少が観察され, 塵のないゾーンを示唆しています.
  • 小さな太陽噴火の微細なプラズマ構造を解明し,磁気流のロープと磁気島を特定した.
  • 大規模な冠状のトポロジーを確認し,冠状のストリーム内のサブストリームを明らかにしました.

結論:

  • パーカー・ソーラー・プローブの観測は 太陽の近くにある 塵のない領域の証拠を提供している.
  • この研究は,これまで観測されていなかった 磁気構造を小さな太陽噴火で解明しました
  • 冠状のストリームは,連続した密度の変動を持つ小さなサブストリームで構成されています.