Hydrogen peroxide on Mars: evidence for spatial and seasonal variations

Encrenaz, Thérèse; Bézard, Bruno; Greathouse, T. K.; Richter, M. J.; Lacy, J. H.; Atreya, S. K.; Wong, Anthony T.; Lebonnois, Sébastien; Lefèvre, Franck; Forget, F.

doi:10.1016/j.icarus.2004.05.008

Cited by 177 publications

(117 citation statements)

References 18 publications

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“…Since 2001, we have been mapping the Martian disk with the TEXES instrument at IRTF, with the prime objective of detecting and mapping hydrogen peroxide (Encrenaz et al 2002) (Encrenaz et al 2004). In addition, we have been using weak transitions of HDO to monitor the water vapor simultaneously (Encrenaz et al 2005).…”

Section: Observations and Data Analysismentioning

confidence: 99%

“…The individual pixel size was 0.368 arcsec and the spatial resolution, after convolution over 3 pixel elements, was 1.1 arcsec. The data reduction and radiance calibration are described in Encrenaz et al (2004Encrenaz et al ( , 2005. Figure 1 shows a part of the spectrum between 1235 and 1237 cm −1 , which includes the HDO transition used in this study as well as several CO 2 transitions of different intensities.…”

Section: Observations and Data Analysismentioning

confidence: 99%

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Water vapor map of Mars near summer solstice using ground-based infrared spectroscopy

Encrenaz¹,

Greathouse

Bézard³

et al. 2010

A&A

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Ground-based spatial mapping of Mars provides a unique way to retrieve the global distribution of minor atmospheric species and to study transient phenomena or possible variations with the local hour. We have obtained an instantaneous map of water vapor on Mars near summer solstice (Ls = 80 • ) using the Texas Echelon Cross Echelle Spectrograph (TEXES) at the NASA Infrared Telescope Facility (IRTF) at Mauna Kea Observatory. Data have been obtained in the 1230-1245 cm −1 range (λ = 8.1 μm), with a spatial resolution of 1.1 arcsec (after convolution) and a spectral resolution of 0.012 cm −1 (R = 10 5 ). The map has been retrieved from the line depth of a weak HDO transition, compared with the line depth of a weak CO 2 nearby transition. The TEXES map exhibits a strong maximum around the northern pole, as expected from previous observations and from climate model predictions. More interestingly, it shows longitudinal variations, both at high northern latitudes and at mid-latitudes, in close agreement with the predictions of the Global Climate Model developed at the Laboratoire de Meteorologie Dynamique (LMD GCM). The inferred water vapor mixing ratio is also in good agreement with the model predictions. The longitudinal variations at mid latitudes show a general enhancement toward the east. They do not seem to be due to the effect of local hour, but can be explained by dynamical effects generated by the topography. The map of surface temperatures, inferred from the continuum flux, is surprisingly different from the map expected from the climate models; the source of this discrepancy is still unclear.

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Section: Observations and Data Analysismentioning

confidence: 99%

Section: Observations and Data Analysismentioning

confidence: 99%

Water vapor map of Mars near summer solstice using ground-based infrared spectroscopy

Encrenaz¹,

Greathouse

Bézard³

et al. 2010

A&A

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“…Astrophysically there have been multiple detections of H2O2 in the atmosphere of Mars (Clancy et al 2004;Encrenaz et al 2004Encrenaz et al , 2012Aoki et al 2015) with seasonal variation, possibly formed by triboelectricity in dust devils and dust storms (Encrenaz et al 2012) and may well act as an agent in the oxidization of the Martian surface. Hydrogen peroxide has also been detected in the atmosphere of Europa (Hand & Brown 2013) in the 3.5 µm region.…”

Section: Introductionmentioning

confidence: 99%

ExoMol line lists – XV. A new hot line list for hydrogen peroxide

Al-Refaie

Polyansky

Ovsyannikov

et al. 2016

Mon. Not. R. Astron. Soc.

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A computed line list for hydrogen peroxide, H 2 16 O 2 , applicable to temperatures up to T = 1250 K is presented. A semi-empirical high accuracy potential energy surface is constructed and used with an ab initio dipole moment surface as input TROVE to compute 7.5 million rotational-vibrational states and around 20 billion transitions with associated Einstein-A coefficients for rotational excitations up to J = 85. The resulting APTY line list is complete for wavenumbers below 6 000 cm −1 (λ < 1.67 µm) and temperatures up to 1250 K. Room-temperature spectra are compared with laboratory measurements and data currently available in the HITRAN database and literature. Our rms with line positions from the literature is 0.152 cm −1 and our absolute intensities agree better than 10%. The full line list is available from the CDS database as well as at www.exomol.com.

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“…It is a key constituent in the gas-and liquid-phase radical chemistry and has an oxidizing potential in the liquid phase. Gas-phase HOOH has been seen in the Martian atmosphere by ground-based observations (Clancy et al 2004;Encrenaz et al 2004). However, recent Mars observations with the Herschel Observatory (Hartogh et al 2010) failed to detect HOOH at levels below those previously seen.…”

Section: Introductionmentioning

confidence: 99%

Detection of interstellar hydrogen peroxide

Bergman

Parise

Liseau

et al. 2011

A&A

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Context. The molecular species hydrogen peroxide, HOOH, is likely to be a key ingredient in the oxygen and water chemistry in the interstellar medium. Aims. Our aim with this investigation is to determine how abundant HOOH is in the cloud core ρ Oph A. Methods. By observing several transitions of HOOH in the (sub)millimeter regime we seek to identify the molecule and also to determine the excitation conditions through a multilevel excitation analysis. Results. We have detected three spectral lines toward the SM1 position of ρ Oph A at velocity-corrected frequencies that coincide very closely with those measured from laboratory spectroscopy of HOOH. A fourth line was detected at the 4σ level. We also found through mapping observations that the HOOH emission extends (about 0.05 pc) over the densest part of the ρ Oph A cloud core. We derive an abundance of HOOH relative to that of H 2 in the SM1 core of about 1 × 10 −10 . Conclusions. To our knowledge, this is the first reported detection of HOOH in the interstellar medium.

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Hydrogen peroxide on Mars: evidence for spatial and seasonal variations

Cited by 177 publications

References 18 publications

Water vapor map of Mars near summer solstice using ground-based infrared spectroscopy

Water vapor map of Mars near summer solstice using ground-based infrared spectroscopy

ExoMol line lists – XV. A new hot line list for hydrogen peroxide

Detection of interstellar hydrogen peroxide

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