Regioselectivity of the photochemical addition of phosphine to unsaturated hydrocarbons in the atmospheres of Jupiter and Saturn

Guillemin, Jean‐Claude; Serre, S. Le; Lassalle, L.

doi:10.1016/s0273-1177(97)00358-x

Cited by 8 publications

(9 citation statements)

References 24 publications

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“…This reaction pathway is consistent with the nature of the products observed starting from ammonia and an alkene. Starting from a dissymmetric alkene, the proposed reaction pathway is consistent with the nature of the more abundant product, the hydrogen radical mainly adding on the less substituted carbon (Guillemin et al, 1995(Guillemin et al, , 1997(Guillemin et al, , 1998. On the contrary, starting from NH 3 and an alkyne, the formation of vinylamine has never been unambiguously evidenced (Ferris et al, 1992) (Scheme 12).…”

Section: Addition Of Nh 3 H 2 S or H 2 O On Alkenes And Alkynesmentioning

confidence: 58%

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Prebiotic, planetary and interstellar chemistry starting from compounds detected in the interstellar medium

Guillemin

Bouyahyi

Riague

2004

Advances in Space Research

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Section: Addition Of Nh 3 H 2 S or H 2 O On Alkenes And Alkynesmentioning

confidence: 58%

“…This latter adds on the C-C multiple bond to form a radical (6), which is also able to abstract a hydrogen from H 2 S (7). A radical chain process thus occurs (Guillemin et al, 1997(Guillemin et al, , 1998. This reaction can be performed with a 254 nm lamp.…”

Section: Addition Of Nh 3 H 2 S or H 2 O On Alkenes And Alkynesmentioning

confidence: 99%

Prebiotic, planetary and interstellar chemistry starting from compounds detected in the interstellar medium

Guillemin

Bouyahyi

Riague

2004

Advances in Space Research

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“…UV photolysis of phosphine in the presence of hydrocarbons could lead to the formation of complicated alkyl-phosphines (Guillemin et al 1997;Guillemin et al 1995). Atmospheres that are prone to high concentrations of hydrocarbon radicals, such as H2-rich atmospheres, could therefore lead to the creation of organophosphine hazes.…”

Section: Solubility and Aerosol Formationmentioning

confidence: 99%

“…The photochemistry of PH3 with radicals originating from other, more exotic, atmospheric species, though likely to be small, is insufficiently studied. For example, photochemistry of PH3 and hydrocarbons, through UV-radiation, could lead to the formation of complicated alkyl-phosphines (Guillemin et al 1997;Guillemin et al 1995), and in consequence increase the probability of hazes. Inclusion of these reactions would increase PH3 destruction rates and hence increase the required surface fluxes for detection; however, since these species are not expected to be dominant radicals, the effect of their inclusion would be minor and should not affect our results.…”

Section: Reaction Network and Haze Formationmentioning

confidence: 99%

Phosphine as a Biosignature Gas in Exoplanet Atmospheres

et al. 2020

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A long-term goal of exoplanet studies is the identification and detection of biosignature gases. Beyond the most discussed biosignature gas O2, only a handful of gases have been considered in detail. Here we evaluate phosphine (PH3). On Earth, PH3 is associated with anaerobic ecosystems, and as such it is a potential biosignature gas in anoxic exoplanets.We simulate the atmospheres of habitable terrestrial planets with CO2-and H2-dominated atmospheres, and find that phosphine can accumulate to detectable concentrations on planets with surface production fluxes of 10 10 -10 14 cm -2 s -1 (corresponding to surface concentrations of 10s of ppb to 100s of ppm), depending on atmospheric composition, and UV irradiation. While high, the surface flux values are comparable to the global terrestrial production rate of methane, or CH4 (10 11 cm -2 s -1 ) and below the maximum local terrestrial PH3 production rate (10 14 cm -2 s -1 ). As with other gases, PH3 can more readily accumulate on low-UV planets, e.g. planets orbiting quiet M-dwarfs or with a photochemically generated UV shield.If detected, phosphine is a promising biosignature gas, as it has no known abiotic false positives on terrestrial planets from any source that could generate the high fluxes required for detection. PH3 also has three strong spectral features such that in any atmosphere scenario one of the three will be unique compared to other dominant spectroscopic molecules. PH3's weakness as a biosignature gas is its high reactivity, requiring high outgassing rates for detectability. We calculate that tens of hours of JWST time are required for a potential detection of PH3. Yet, because PH3 is spectrally active in the same wavelength regions as other atmospherically important molecules (such as H2O and CH4), searches for PH3 can be carried out at no additional observational cost to searches for other molecular species relevant to characterizing exoplanet habitability.

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“…It must also be pointed out that PH 3 has been found in Saturn, 25 Jupiter, 26 and other planets 27 where it is expected to undergo addition reactions to unsaturated hydrocarbons. 28 The existence of PH 3 in IRC + 10 216 raises the question of a) Author to whom correspondence should be addressed. Electronic mail:…”

Section: Introductionmentioning

confidence: 99%

The dynamics of the C + PH3 reaction: A theoretical study

Rey-Villaverde

Álvarez‐Barcia

Flores

2012

The Journal of Chemical Physics

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The C + PH(3) reaction is one of the simplest gas-phase processes which can produce molecular species containing P-C bonds. It could be of astrophysical importance and a reference for other phosphine reactions with carbon-containing molecular radicals. The dynamical aspects have been studied theoretically by quasi-classical trajectory methods in order to determine its rate as a function of the temperature, the branching ratios, and the molecular mechanisms. We have obtained a T(0.2) dependence of the capture rate. The total rate is affected by the existence of relatively high-lying saddle points for the isomerization of the CPH(3) complex but get a value of 0.82·10(-10) cm(3) s(-1) at 300 K, which is considered quite high for a neutral-neutral reaction and higher than those of similar reactions. Moreover, the total rate presents a weak dependence with the temperature. Our results indicate that several products containing P-C bonds are formed, the main reaction channel being the generation of HPCH + H.

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Regioselectivity of the photochemical addition of phosphine to unsaturated hydrocarbons in the atmospheres of Jupiter and Saturn

Cited by 8 publications

References 24 publications

Prebiotic, planetary and interstellar chemistry starting from compounds detected in the interstellar medium

Prebiotic, planetary and interstellar chemistry starting from compounds detected in the interstellar medium

Phosphine as a Biosignature Gas in Exoplanet Atmospheres

The dynamics of the C + PH3 reaction: A theoretical study

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