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Ultraviolet and Visible (UV–Vis) Spectroscopy: Overview01:02

Ultraviolet and Visible (UV–Vis) Spectroscopy: Overview

Ultraviolet–visible (UV–visible or UV–Vis) spectroscopy is an analytical technique that investigates the interaction between matter and UV–Vis light within the electromagnetic spectrum. This method is widely used for its versatility, simplicity, and relatively quick data acquisition, making it valuable for both qualitative and quantitative analysis. When UV–Vis radiation passes through a material,  molecules absorb light depending on the energy required for electronic transitions. As a result...
Atomic Emission Spectroscopy: Interference01:30

Atomic Emission Spectroscopy: Interference

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,...
Atomic Emission Spectroscopy: Overview01:20

Atomic Emission Spectroscopy: Overview

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...
Emission Spectra02:39

Emission Spectra

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.
Infrared (IR) Spectroscopy: Overview01:09

Infrared (IR) Spectroscopy: Overview

When electromagnetic radiation passes through a material, atoms or molecules transition from a lower to a higher energy state by absorbing radiation corresponding to the energy difference between the two states. The absorption of infrared (IR) radiation causes transitions between vibrational energy levels in a molecule. Therefore, IR spectroscopy is a useful analytical tool for determining the molecular structure of molecules.
Different compounds display unique properties due to their...
Atomic Emission Spectroscopy: Lab01:29

Atomic Emission Spectroscopy: Lab

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...

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Bringing the Visible Universe into Focus with Robo-AO
10:35

Bringing the Visible Universe into Focus with Robo-AO

Published on: February 12, 2013

イオの日食に対する大気反応:UVオーロラの観測

K D Retherford1, J R Spencer, S A Stern

  • 1Southwest Research Institute, San Antonio, TX 78228, USA. KRetherford@swri.edu

Science (New York, N.Y.)
|October 13, 2007
PubMed
まとめ

木星の衛星イオのオーロラの明るさと形状は,宇宙船ニューホライゾンズを使って研究されました. 火山はイオの昼間の大気の1~3%を占め,木星の磁気圏との相互作用に影響を与えます.

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Published on: February 12, 2013

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科学分野:

  • 惑星科学は惑星科学である.
  • 宇宙物理学 宇宙物理学
  • 天体物理学 天体物理学

背景:

  • 木星の火山の月イオは薄い大気を持ち,木星の磁気圏とダイナミックに相互作用しています.
  • イオのオーロラ放射は,大気組成と磁気圏の相互作用に関する洞察を提供します.

研究 の 目的:

  • イオの大気に対する火山活動と昇華の相対的な貢献を調査する.
  • エクリプス中のイオのオーロラ放射を分析し,大気密度の変動を理解する.
  • 木星の磁気圏とイオの電動相互作用に対する火山の羽根の影響を決定する.

主な方法:

  • 2007年春,イオの4回の日食観測中にニューホライゾン (NH) アリスの紫外線スペクトロスコーピーを利用しました.
  • 同時期にハッブル宇宙望遠鏡の紫外線画像と相関したNH紫外線データ.
  • 観測データをIoのオーロラ放射の詳細なシミュレーションと比較した.

主要な成果:

  • オーロラ光の明るさと形状は,日食の入出後に大きく変化し,大気源の貢献のシフトを示しています.
  • 様々な幾何学的な点での観測された明るさの差異は,イオの昼側と夜側の大気間の密度の大きな差異を示唆しています.
  • 遠紫外線のオーロラ形態は,火山の羽根がイオの磁気圏と木星の磁気圏との電動的結合に与える影響を強調した.

結論:

  • 火山の噴出源は,イオの昼間の大気の1〜3%を供給すると推定されています.
  • 大気密度は,イオの昼側と夜側との劇的な違いを示しています.
  • イオの羽根は磁気圏の相互作用において重要な役割を果たしています.