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Related Concept Videos

The Phosphorus Cycle01:21

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Unlike carbon, water, and nitrogen, phosphorus is not present in the atmosphere as a gas. Instead, most phosphorus in the ecosystem exists as compounds, such as phosphate ions (PO43-), found in soil, water, sediment and rocks. Phosphorus is often a limiting nutrient (i.e., in short supply). Consequently, phosphorus is added to most agricultural fertilizers, which can cause environmental problems related to runoff in aquatic ecosystems.
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Analysis of Volatile and Oxidation Sensitive Compounds Using a Cold Inlet System and Electron Impact Mass Spectrometry
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Phosphine on Venus Cannot Be Explained by Conventional Processes.

William Bains1,2, Janusz J Petkowski1, Sara Seager1,3,4

  • 1Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, Massachusetts, USA.

Astrobiology
|July 20, 2021
PubMed
Summary
This summary is machine-generated.

The detection of phosphine gas in Venus's atmosphere is unexpected. Current models cannot explain its presence, suggesting unknown geochemical or biological processes may be responsible.

Keywords:
Biosignature gasLifePhosphinePhotochemistryThermodynamicsVenus

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Area of Science:

  • Astrobiology
  • Planetary Science
  • Atmospheric Chemistry

Background:

  • Recent candidate detection of phosphine (PH3) in Venus's atmosphere at ~1 ppb.
  • Phosphorus-containing species have not been previously modeled for Venus.
  • The origin of atmospheric phosphine on Venus is currently unexplained.

Purpose of the Study:

  • To investigate potential formation pathways for phosphine in the Venusian environment.
  • To assess known chemical and geochemical processes as sources of Venusian phosphine.
  • To evaluate phosphine as a potential biosignature on Venus.

Main Methods:

  • Modeling of phosphorus-containing species in Venus's atmosphere.
  • Exploration of gas-phase reactions, photochemistry, and geochemical reactions.
  • Investigation of potential phosphine formation in the atmosphere, clouds, haze, surface, and subsurface.

Main Results:

  • No known geochemical or photochemical pathways adequately explain the observed ppb levels of phosphine.
  • Existing models of Venusian atmospheric chemistry are insufficient to account for the phosphine detection.
  • The presence of phosphine suggests unknown processes may be occurring on Venus.

Conclusions:

  • If confirmed, Venusian phosphine likely originates from unknown geochemistry, photochemistry, or biological activity.
  • Phosphine on Venus could represent a biosignature, warranting further investigation.
  • The findings emphasize the need for in situ missions to Venus for sample analysis and atmospheric characterization.