Phosphorus in the Clouds of Venus: Potential for Bioavailability

Milojevic, Tetyana; Treiman, Allan H.; Limaye, S. S.

doi:10.1089/ast.2020.2267

Cited by 19 publications

(9 citation statements)

References 131 publications

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“…As the main constituent of the Jovian atmospheres is molecular hydrogen, essentially all of the phosphorus is present in the form of PH 3 − In giant planets, such as Jupiter and Saturn, phosphorus is found in the PH 3 form, and the volume mixing ratio is about 10 –6 on Jupiter. , However, the presence of such element in the clouds decks of Venus’s atmosphere is still under debate. ,,− Though PH 3 is not the most thermodynamically favorable form of gas-phase phosphorus at temperatures of the Venus atmosphere, PH 3 formed in the hot deep layers should be brought to the top of the atmosphere through convective transport.…”

Section: Implications For Astrochemistrymentioning

confidence: 99%

Phosphine Reactivity and Its Implications for Pyrolysis Experiments and Astrochemistry

Baptista

Almeida

2023

J. Phys. Chem. A

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Despite the importance of phosphorus-bearing molecules for life and their abundance outside Earth, the chemistry of those compounds still is poorly described. The present study investigates phosphine (PH3) decomposition and formation pathways. The reactions studied include phosphine thermal dissociation, conversion into PO(2Π), PN(1Σ+), and reactions in the presence of H2O+. The thermodynamic and rate coefficients of all reactions are calculated in the range of 50–2000 K considering the CCSD(T)/6-311G(3df,3pd)//ωB97xD/6-311G(3df,3pd) electronic structure data. The rate coefficients were calculated by RRKM and semiclassical transition-state theory (SCTST). According to our results, PH3 is stable to thermal decomposition at T < 100 K and can be formed promptly by a reaction network involving PH(3Σ–), PO(2Π), and PN(1Σ+). In the presence of radiation or ions, PH3 is readily decomposed. For this reason, it should be mainly associated with dust grains or icy mantles to be observed under the physical conditions prevailing in the interstellar medium (ISM). The intersystem crossing associated with the dissociation of the isomers PON, NPO, and PNO is accessed by multireference methods, and its importance for the gas-phase PH3 formation/destruction is discussed. Also, the implications of the present outcomes on phosphorus astrochemistry are highlighted.

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Section: Implications For Astrochemistrymentioning

confidence: 99%

Phosphine Reactivity and Its Implications for Pyrolysis Experiments and Astrochemistry

Baptista

Almeida

2023

J. Phys. Chem. A

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“…By these metrics, hypothetical life in venusian aerosols may be within the bounds of temperature, pressure, and pH (Grinspoon and Bullock, 2007;Nicholson et al, 2010); radiation (Schulze-Makuch and Irwin, 2002;Dartnell et al, 2015); C, H, N, O, and S, with some evidence for P (Limaye et al, 2021a;Milojevic et al, 2021;Mogul et al, 2021); and energy sources (photonic and/or oxidation-reduction potential, Limaye et al 2018;Mogul et al 2021b). Seager et al (2020) argue that because the pH scale becomes highly compressed at extreme acid (or base) concentrations, the Hammett acidity function (H 0 ) is a more representative metric for the Venus aerosols' acid activity.…”

Section: Life In the Cloudsmentioning

confidence: 99%

The Habitability of Venus and a Comparison to Early Earth

Westall

Höning

Avice

et al. 2022

Preprint

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HAL is a multi-disciplinary open access archive for the deposit and dissemination of scientific research documents, whether they are published or not. The documents may come from teaching and research institutions in France or abroad, or from public or private research centers. L'archive ouverte pluridisciplinaire HAL, est destinée au dépôt et à la diffusion de documents scientifiques de niveau recherche, publiés ou non, émanant des établissements d'enseignement et de recherche français ou étrangers, des laboratoires publics ou privés.

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“…In the giant planets, phosphorus is found in the PH 3 form, and the volume mixing ratio is about 10-6 on Jupiter [86,87]. However, the presence of such element in the deck clouds of Venus is still under debate [74,[88][89][90][91]. Though PH 3 is not the most thermodynamically favorable form of gas-phase phosphorus at temperatures of the Venus atmosphere, PH 3 formed in the hot deep layers should be brought to the top of the atmosphere through convective transport.…”

Section: Implications For Astrochemistrymentioning

confidence: 99%

Phosphine reactivity and its implications for pyrolysis experiments and astrochemistry

Baptista

Almeida

2022

Preprint

View full text Add to dashboard Cite

Despite the importance of phosphorus-bearing molecules for life and their abundance outside Earth, the chemistry of those compounds still is poorly described. The present study investigated phosphine (PH3) decomposition and formation pathways. The reactions studied include phosphine thermal dissociation, conversion into PO, PN, and reactions in the presence of H2O+. The thermodynamic and rate coefficients of all reactions were calculated in the range of 50 – 2000 K considering the CCSD(T)/6-311G(3df,3pd)//B97xD/6-311G(3df,3pd) electronic structure data. The rate coefficients were calculated by RRKM and SCTST theories. According to the results, PH3 is stable due to thermal decomposition at T < 100 K but can be formed promptly by a reaction mechanism involving PH, PO, and PN. In the presence of radiation or ions, PH3 is readily decomposed. For this reason, it should be mainly associated with dust grains or icy mantles to be observed. The intersystem crossing associated with the dissociation of the isomers PON, NPO, and PNO was accessed by multireference methods, and its importance for the gas-phase PH3 formation/destruction was discussed. Also, the impact of the present outcomes on the phosphorus space chemistry was highlighted.

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Phosphorus in the Clouds of Venus: Potential for Bioavailability

Abstract: Aerosol phase elements such as phosphorus (P), sulfur (S), and metals including iron (Fe) are essential nutrients that could help sustain potential biodiversity in the cloud deck of Venus. While the presence of S and Fe in the venusian cloud deck has been broadly discussed (

Cited by 19 publications

References 131 publications

Phosphine Reactivity and Its Implications for Pyrolysis Experiments and Astrochemistry

Phosphine Reactivity and Its Implications for Pyrolysis Experiments and Astrochemistry

The Habitability of Venus and a Comparison to Early Earth

Phosphine reactivity and its implications for pyrolysis experiments and astrochemistry

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