Ultraviolet absorption cross sections of hydrogen peroxide

Lin, C. L.; Rohatgi, N.; DeMore, W. B.

doi:10.1029/gl005i002p00113

Cited by 85 publications

(30 citation statements)

References 9 publications

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“…As to the H 2 O 2 photolysis the simulation was carried out considering a photolysis constant of 5.61 Â 10 À 4 s À 1 obtained by a cross section [37] of 7.4 Â 10 À 20 cm 2 and a quantum yield [38] of 0.5. Moreover, the reactions (3) and (4) were taken into account.…”

Section: Theoretical Explanation Of the Analytical Signalmentioning

confidence: 99%

A new electrochemical sensor for OH radicals detection

Gualandi

Tonelli

2013

Talanta

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Section: Theoretical Explanation Of the Analytical Signalmentioning

confidence: 99%

A new electrochemical sensor for OH radicals detection

Gualandi

Tonelli

2013

Talanta

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“…Hydrogen peroxide absorbs UV radiation (26), so if our identification is correct we expect (6) a corresponding absorption signature to be present in Galileo UVS spectra (27). Disk-resolved UVS measurements (obtained concurrently with the NIMS observations) were com- Spatially resolved infrared and ultraviolet wavelength spectra of Europa's leading, anti-jovian quadrant observed from the Galileo spacecraft show absorption features resulting from hydrogen peroxide.…”

mentioning

confidence: 91%

Hydrogen Peroxide on the Surface of Europa

Carlson

Anderson

Johnson

et al. 1999

Science

290

203

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Spatially resolved infrared and ultraviolet wavelength spectra of Europa's leading, anti-jovian quadrant observed from the Galileo spacecraft show absorption features resulting from hydrogen peroxide. Comparisons with laboratory measurements indicate surface hydrogen peroxide concentrations of about 0.13 percent, by number, relative to water ice. The inferred abundance is consistent with radiolytic production of hydrogen peroxide by intense energetic particle bombardment and demonstrates that Europa's surface chemistry is dominated by radiolysis.

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“…The combined experimental photoabsorption cross sections of Lin et al (1978) and Suto & Lee (1983) extend from 105 to 195 nm, with the absorption at the longest wavelength being very small (less than 10 −21 cm 2 ) and likely to be temperature dependent. A photoionisation cross section was assembled by combining absolute and relative measurements of H 2 O + 2 production (Dodson et al 2015;Litorja & Ruscic 1998) and assuming a low production of fragmented ions.…”

Section: H 2 O 2 -Hydrogen Peroxidementioning

confidence: 99%

Photodissociation and photoionisation of atoms and molecules of astrophysical interest

Heays

Bosman

Dishoeck

2017

A&A

442

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A new collection of photodissociation and photoionisation cross sections for 102 atoms and molecules of astrochemical interest has been assembled, along with a brief review of the basic physical processes involved. These have been used to calculate dissociation and ionisation rates, with uncertainties, in a standard ultraviolet interstellar radiation field (ISRF) and for other wavelength-dependent radiation fields, including cool stellar and solar radiation, Lyman-α dominated radiation, and a cosmic-ray induced ultraviolet flux. The new ISRF rates generally agree within 30% with our previous compilations, with a few notable exceptions. Comparison with other databases such as PHIDRATES is made. The reduction of rates in shielded regions was calculated as a function of dust, molecular and atomic hydrogen, atomic C, and self-shielding column densities. The relative importance of these shielding types depends on the atom or molecule in question and the assumed dust optical properties. All of the new data are publicly available from the Leiden photodissociation and ionisation database. Sensitivity of the calculated rates to variation of temperature and isotope, and uncertainties in measured or calculated cross sections, are tested and discussed. Tests were conducted on the new rates with an interstellar-cloud chemical model, and find general agreement (within a factor of two) in abundances obtained with the previous iteration of the Leiden database assuming an ISRF, and order-of-magnitude variations assuming various kinds of stellar radiation. The newly parameterised dust-shielding factors makes a factor-of-two difference to many atomic and molecular abundances relative to parameters currently in the UDfA and KIDA astrochemical reaction databases. The newly-calculated cosmic-ray induced photodissociation and ionisation rates differ from current standard values up to a factor of 5. Under high temperature and cosmic-ray-flux conditions the new rates alter the equilibrium abundances of abundant dark cloud abundances by up to a factor of two. The partial cross sections for H 2 O and NH 3 photodissociation forming OH, O, NH 2 and NH are also evaluated and lead to radiation-field-dependent branching ratios.

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Ultraviolet absorption cross sections of hydrogen peroxide

Cited by 85 publications

References 9 publications

A new electrochemical sensor for OH radicals detection

A new electrochemical sensor for OH radicals detection

Hydrogen Peroxide on the Surface of Europa

Photodissociation and photoionisation of atoms and molecules of astrophysical interest

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