The chemistry of phosphorus in dense interstellar clouds

Thorne, L. R.; Anicich, V. G.; Prasad, S. S.; Huntress, W. T.

doi:10.1086/161977

Cited by 88 publications

(61 citation statements)

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“…Therefore the ratio kcp ~ 1.5 kps ~ 2.6 kpH suggests a triple bond between the C and P atoms in contrast to a double bond character for the PS molecule and a single bond for PH. This is conforms with Thorne et al [1], who reported that the CP radical has the highest bond energy among various phosphorus containing molecules. In comparison, the CN triple bond produces = 1.0B10 9 (with ^0 cN = 2062.13 cm" 1 [15]) about twice the value of kcp.…”

Section: J = N + S and F = J + Isupporting

confidence: 93%

“…Thorne et al estimated bond energies of several simple phosphorus containing molecules like PH, PH 2 , P 2 , CP, etc. and they conclude that the CP radical has the highest bond energy among them [1]. In the laboratory, the CP radical was first studied by Herzberg in 1930 [2], who identified this molecule via its electronic B 2 Z + -X 2 Z + transition.…”

Section: Introductionmentioning

confidence: 99%

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CP's Triple-bond Strength Experienced in its THz Spectrum

Klein

Klisch

Winnewisser

et al. 1999

Zeitschrift Für Naturforschung A

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The submillimeter-wave rotational spectrum of the CP radical in the electronic and vibrational ground state (X 2 Z + ) was recorded in the frequency region between 572 GHz and 1.05 THz, covering rotational quantum numbers from N = 11 up to 21. The CP radical has been produced by discharging CH4 over red phosphorus buffered with Ar at liquid nitrogen temperature. Analysis of the new rotational data of CP together with those available in the literature allows the derivation of an accurate set of molecular constants, including rotational, BQ = 23859.91521(28) MHz and the centrifugal distortion constant Do = 39.8140(19) kHz, the fine structure and hyperfine structure parameters. The stiffness of the CP bond can be inferred by requiring only one distortion constant Do to fit the measured rotational spectrum.

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Section: J = N + S and F = J + Isupporting

confidence: 93%

Section: Introductionmentioning

confidence: 99%

CP's Triple-bond Strength Experienced in its THz Spectrum

Klein

Klisch

Winnewisser

et al. 1999

Zeitschrift Für Naturforschung A

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“…The gas-phase reactions were taken from the UMIST database (McElroy et al 2013), which includes the original network for phosphorus of Millar (1991). This network is based on the early experimental work of Thorne et al (1983Thorne et al ( , 1984 and Smith et al (1989), and only ∼30% of the reactions have rate coefficients measured in the laboratory. We have also added the chemical reactions involving PH 3 from the chemical network of Charnley & Millar (1994), who took the rate coefficients of the neutral-neutral reactions H + PH n (n=1-3) from Kaye & Strobel (1983) following the experimental data of Lee et al (1976).…”

Section: Chemical Modeling Of P-bearing Moleculesmentioning

confidence: 99%

The Chemistry of Phosphorus-bearing Molecules under Energetic Phenomena

Jiménez-Serra

Viti

Quénard

et al. 2018

ApJ

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For decades, the detection of phosphorus-bearing molecules in the interstellar medium was restricted to high-mass star-forming regions (e.g., SgrB2 and Orion KL) and the circumstellar envelopes of evolved stars. However, recent higher-sensitivity observations have revealed that molecules such as PN and PO are present not only toward cold massive cores and low-mass star-forming regions with PO/PN ratios 1 but also toward the giant molecular clouds in the Galactic center known to be exposed to highly energetic phenomena such as intense UV radiation fields, shock waves, and cosmic rays. In this paper, we carry out a comprehensive study of the chemistry of phosphorus-bearing molecules across different astrophysical environments that cover a range of physical conditions (cold molecular dark clouds, warm clouds, and hot cores/hot corinos) and are exposed to different physical processes and energetic phenomena (proto-stellar heating, shock waves, intense UV radiation, and cosmic rays). We show how the measured PO/PN ratio (either 1, as in, e.g., hot molecular cores, or 1, as in UV strongly illuminated environments) can provide constraints on the physical conditions and energetic processing of the source. We propose that the reaction P+OH→PO+H, not included in previous works, could be an efficient gas-phase PO formation route in shocks. Our modeling provides a template with which to study the detectability of P-bearing species not only in regions in our own Galaxy but also in extragalactic sources.

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“…The few theoretical models devoted to P-chemistry disagree in both the chemical formation pathways and the predictions of the abundances of PO and PN. While some works (Millar et al 1987;Adams et al 1990;Charnley & Millar 1994) suggest that PN should be more abundant than PO, other studies involving theoretical modeling and laboratory experiments (e.g., Thorne et al 1984) predict that P should be found mainly in the form of PO.…”

Section: Introductionmentioning

confidence: 98%

The First Detections of the Key Prebiotic Molecule Po in Star-Forming Regions

Rivilla

Fontani

Beltrán

et al. 2016

ApJ

110

135

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Phosphorus is a crucial element in biochemistry, in particular the P−O bond, which is key in the formation of the backbone of deoxyribonucleic acid. So far, PO has only been detected toward the envelope of evolved stars, but never toward star-forming regions. We report the first detection of PO toward two massive star-forming regions, W51 e1/e2 and W3(OH), using data from the IRAM 30 m telescope. PN has also been detected toward the two regions. The abundance ratio PO/PN is 1.8 and 3 for W51 and W3(OH), respectively. Our chemical model indicates that the two molecules are chemically related and are formed via gas-phase ion-molecule and neutralneutral reactions during cold collapse. The molecules freeze out onto grains at the end of the collapse and desorb during the warm-up phase once the temperature reaches ∼35 K. Similar abundances of the two species are expected during a period of ∼5 × 10 4 yr at the early stages of the warm-up phase, when the temperature is in the range 35-90 K. The observed molecular abundances of 10 −10 are predicted by the model if a relatively high initial abundance of 5 × 10 −9 of depleted phosphorus is assumed.

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The chemistry of phosphorus in dense interstellar clouds

Cited by 88 publications

References 0 publications

CP's Triple-bond Strength Experienced in its THz Spectrum

CP's Triple-bond Strength Experienced in its THz Spectrum

The Chemistry of Phosphorus-bearing Molecules under Energetic Phenomena

The First Detections of the Key Prebiotic Molecule Po in Star-Forming Regions

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