関連する実験動画
Updated: Jul 12, 2026

11:34
Scattering And Absorption of Light in Planetary Regoliths
Published on: July 1, 2019
まとめ
パイオニア・ヴェーナスの太陽流量放射計の測定は,硫黄雲のモデルに挑戦しています. 一貫した流量プロフィールには,おそらく塵から,金星に衝撃を与える上部雲の追加の吸収が必要です.
科学分野:
- 惑星科学は惑星科学である.
- 大気物理学 大気物理学
- 放射能の移転について
背景:
- ヴィーナス大探査機 (Pioneer Venus Large Probe) の大型太陽流量放射計 (LSFR) データは,ヴィーナの大気中のエネルギーバランスに関する重要な洞察を提供します.
- 以前の大気モデルでは,しばしば硫黄で構成された雲粒子が想定されていたが,直接的な流量測定では再評価が必要である.
- 金星の雲の構成と放射性特性を理解することは,その大気構造と熱のバランスを制限する鍵です.
研究 の 目的:
- パイオニア・ヴェーナスのLSFRからのin-situ太陽流量測定と,ヴェーナスのモデル大気の理論的計算を比較する.
- 金星の雲の組成,特に硫黄と潜在的な代替吸収体の役割について,放射性フローの決定において調査する.
- 測定されたフローが,表面温度と断続率を含む,金星の大気熱構造に及ぼす影響を評価する.
主な方法:
- LSFRで測定された太陽光流の比較と,さまざまな雲の粒子組成 (硫黄,塵) を含む放射性転送モデル.
- 狭帯域 (0.5900.665 μm) とブロードバンドのスペクトルデータを分析して,吸収光学深さとスペクトル特性を決定する.
- 観測された可視流量,雲の不透明性,水蒸気量の測定を用いた熱バランス計算により,大気温プロファイルが得られます.
主要な成果:
- 大量の硫黄雲粒子を想定したモデルは,強い短波長吸収により,LSFR測定と一致しないフクロスプロファイルを生成しました.
- 小さな硫黄粒子を持つモデルには,LSFRデータと一致する追加の上層雲吸収源が必要でした; これは,塵または強い吸収帯である可能性があります.
- 視界流量測定は,高表面温度と中部雲内のコンベクティブ・ラップスレートを示唆し,サブアディアバティック領域は ~35kmまで広がっています.
結論:
- 金星の雲の組成は複雑で,硫黄が唯一の吸収物質ではない可能性があり,追加の吸収種 (例えば,塵) が可能性が高い.
- 観測された放射性流は,特に上層雲の性質と放射性バランスに関する,金星の大気モデルの修正を必要とします.
- 精密な流量測定は,金星の熱構造を決定し,その大気動力学と進化を理解するために重要である.
関連する概念動画
Light as Energy
The energy required to carry out photosynthesis is light— typically electromagnetic radiation from the sun. The range of all possible wavelengths is known as the electromagnetic spectrum.
Photons
A photon is a discrete electromagnetic particle or bundle of energy. Photons are characterized by their frequency, wavelength, and amplitude, similar to the properties of a wave. Waves with higher frequencies transmit more energy and have shorter wavelengths than longer wavelengths that transmit less...
Photons
A photon is a discrete electromagnetic particle or bundle of energy. Photons are characterized by their frequency, wavelength, and amplitude, similar to the properties of a wave. Waves with higher frequencies transmit more energy and have shorter wavelengths than longer wavelengths that transmit less...
Absorption of Radiation
The rate of heat transfer by emitted radiation is described by the Stefan-Boltzmann law of radiation:
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...
Energy Transfer in Chemical Reactions
Chemical reactions require sufficient energy to cause the matter to collide with enough precision and force that old chemical bonds can be broken and new ones formed. In general, kinetic energy is the form of energy powering any type of matter in motion. Imagine a person building a brick wall. The energy it takes to lift and place one brick on top of another is the kinetic energy—the energy matter possesses because of its motion. Once the wall is in place, it stores potential energy. Potential...
UV–Vis Spectroscopy of Conjugated Systems
Organic compounds with conjugated double bonds show strong absorption features in the UV–visible region of the electromagnetic spectrum attributed to π → π* electronic excitations. Generally, a UV–vis absorption spectrum is recorded as a plot of absorbance vs wavelength. The wavelength of maximum absorbance, which manifests as a peak in the absorption spectrum, is denoted as λmax.
One of the factors influencing λmax is the extent of conjugation in the...
One of the factors influencing λmax is the extent of conjugation in the...
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)...
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)...

