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相关概念视频

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...
UV–Vis Spectrometers01:14

UV–Vis Spectrometers

The absorbance of UV and visible (UV–visible) radiations is measured using a UV–visible spectrophotometer. Deuterium lamps, which emit UV radiation, and tungsten lamps, which produce radiation in the visible region, are used as light sources in UV–visible spectrophotometers. A monochromator or prism is used for diffraction grating, i.e., to split the incoming radiation into different wavelengths. A system of slits is used to focus the desired wavelength on the sample cell. Samples for...
UV–Vis Spectroscopy: Molecular Electronic Transitions01:16

UV–Vis Spectroscopy: Molecular Electronic Transitions

In Ultraviolet–Visible (UV–Vis) spectroscopy, the absorption of electromagnetic radiation is used to probe the electronic structure of molecules. This technique provides insights into molecular electronic transitions, particularly the movement of electrons between different molecular orbitals. Radiation is absorbed if the energy of the electromagnetic radiation passing through the molecule is precisely equal to the energy difference between the excited and ground states. During this process,...
UV–Vis Spectrum01:30

UV–Vis Spectrum

When light passes through a substance, a portion of the light is absorbed while the remaining light is reflected or transmitted. If the molecule absorbs light between the wavelengths of 180–400 nm range, the UV spectrum is obtained, and if it absorbs light in the 400–780 nm wavelength range, the visible spectrum is obtained.     
The UV–Vis spectrum of a molecule is the plot of its absorbance versus wavelength. The plot is drawn by taking molar absorptivity (ε) or log ε on the y-axis (ordinate)...
UV–Vis Spectroscopy: Beer–Lambert Law01:09

UV–Vis Spectroscopy: Beer–Lambert Law

The Beer-Lambert law describes the relationship between absorbance and concentration, which combines the principles established by scientists Johann Heinrich Lambert and August Beer. Lambert's law states that when light passes through a medium, the loss in intensity is directly proportional to the original intensity and the path length of the light. Beer's law proposed that the transmittance of a solution remains constant if the product of concentration and path length is constant. The modern...
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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相关实验视频

Updated: Jul 12, 2026

Assays to Detect UV-reflecting Structures and Determine their Importance in Mate Preference using the Sailfin Molly Poecilia latipinna
06:41

Assays to Detect UV-reflecting Structures and Determine their Importance in Mate Preference using the Sailfin Molly Poecilia latipinna

Published on: September 14, 2016

马里纳9号紫外线光谱仪实验:恒星观测

C F Lillie, R C Bohlin, M R Molnar

    Science (New York, N.Y.)
    |January 21, 1972
    PubMed
    概括

    早期类型恒星的紫外线光谱揭示了关键的元素线. 马里纳9号的数据显示,能量分布比之前的观测低约20%,影响了恒星天体物理学研究.

    科学领域:

    • 天文学和天体物理学
    • 恒星光谱学 恒星光谱学

    背景情况:

    • 早期类型的恒星对于理解恒星进化和银河系组成至关重要.
    • 紫外线 (UV) 光谱学为恒星大气和组成提供了独特的见解.

    研究的目的:

    • 为了获得1100-2000安格斯特罗姆范围内早期类型恒星的光电光谱.
    • 确定突出的光谱线并分析这些恒星的绝对能量分布.

    主要方法:

    • 利用Mariner 9紫外线光谱仪捕获恒星光谱.
    • 专注于1100-2000安格斯特罗姆波长地区.

    主要成果:

    • 成功确定了I (H I),IV (Si IV) 和碳IV (C IV) 的共振线.
    • 从碳II (C II),碳III (C III),III (Si III),铁II (Fe II) 和IV (N IV) 中检测到的光谱特征.
    • 获得的绝对能量分布大约比OAO-2在1200-2000安格斯特罗姆范围内获得的能量分布低20%.

    结论:

    • 这项研究为早期类型恒星提供了有价值的紫外线光谱数据.
    • 与以前的任务相比,能量分布的差异需要进一步研究观察方法和校准.

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