External supply of oxygen to the atmospheres of the giant planets

Feuchtgruber, H.; Lellouch, E.; Graauw, Th. de; Bézard, Bruno; Encrenaz, Th.; Griffin, Matthew Joseph

doi:10.1038/38236

Cited by 223 publications

(233 citation statements)

References 30 publications

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“…Recent modeling of the processes taking place in the solar nebula are compatible with the deuterium enrichment with respect to the protosolar D/H ratio either measured in LL3 meteorites and comets (Mousis et al 2002;Eberhardt et al 1995;Bockelée-Morvan et al 1998;Meier et al 1998) or estimated from solar system outer planets HD measurements (Feuchtgruber et al 1999), below the 10 −3 limit. These values are much lower than the dark cloud values for other species (≤a few 10 −2 ).…”

Section: A Possible Scenario For Deuterium Enrichment?mentioning

confidence: 66%

Revisiting the solid HDO/H$_\mathsf{2}$O abundances

Dartois

Thi

Geballe

et al. 2003

A&A

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Abstract. We revisit the reported detection and upper limits on HDO in ice mantles present in the molecular cloud environments of the massive young protostars Gl 2136 and W33 A, using independent VLT-ISAAC and UKIRT-CGS4 spectroscopic observations. We also present VLT and UKIRT spectra of RAFGL 7009 near the HDO absorption wavelength and reanalyze the ISO-SWS spectral data for NGC 7538 IRS9, Orion-BN and S140. We demonstrate that the previously reported detections of HDO in W33 A and NGC 7538 IRS9 are incorrect. We present an in-depth analysis that shows that, besides the sensitivity limits, detection of low levels of HDO is difficult in amorphous ice mantles when features from solid methanol, a common grain mantle constituent, are present. We discuss the specific problems arising in the ISO data in this wavelength range for NGC 7538 IRS9. Using VLT-ISAAC observations, we also investigate the HDO/H 2 O ratio toward the intermediate mass stars IRAS 05329-0728 and IRAS 08448-4343. Our derived upper limits for the D/H ratio in water ice range from HDO/H 2 O < 1% to 0.2% in the different sources, and we discuss these limits in comparison with values derived in other environments.

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Section: A Possible Scenario For Deuterium Enrichment?mentioning

confidence: 66%

Revisiting the solid HDO/H$_\mathsf{2}$O abundances

Dartois

Thi

Geballe

et al. 2003

A&A

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“…The similar H 2 O fluxes per unit area into the four giant planets and Titan (Feuchtgruber et al 1997;Coustenis et al 1998;Moses et al 2000), combined with the rather constant dust flux (∼3×10 −18 g cm −2 s −1 ) measured in interplanetary space beyond 5 AU (Landgraf et al 2002) have been regarded as evidence that micrometeoroids -interplanetary (IDPs) or interstellar -are the dominant source (Moses et al 2000). Along with the evidence that the H 2 O present in Jupiter's atmosphere results from the Shoemaker-Levy 9 1994 impact -and that CO in Jupiter, Saturn, and Neptune Cavalié et al 2010;Lellouch et al 2005) also result from ancient cometary impacts -our inference that Enceladus is a quantitatively viable source of Saturn's water clearly shifts the paradigm towards local or sporadic sources playing a more important role.…”

Section: Discussion and Implications For The Source Of Water In Saturmentioning

confidence: 99%

“…Emission lines due to water vapor in the far-infrared spectrum (λ > 30 μm) of the giant planets and Titan, first discovered by ISO (Feuchtgruber et al 1997;Coustenis et al 1998) prove the existence of an external supply of water to these reducing atmospheres. At Saturn and Jupiter, spectrally resolved observations of the fundamental 1 10 -1 01 line of ortho-H 2 O at 557 GHz (538 μm), obtained by SWAS in September 1999 (Bergin et al 2000), indicated a ∼10% contrast emission with ∼20 km s −1 width.…”

Section: Observations and Initial Interpretationmentioning

confidence: 99%

Direct detection of the Enceladus water torus withHerschel

Hartogh

Lellouch

Moreno

et al. 2011

A&A

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Cryovolcanic activity near the south pole of Saturn's moon Enceladus produces plumes of H 2 O-dominated gases and ice particles, which escape and populate a torus-shaped cloud. Using submillimeter spectroscopy with Herschel, we report the direct detection of the Enceladus water vapor torus in four rotational lines of water at 557, 987, 1113, and 1670 GHz, and probe its physical conditions and structure. We determine line-of-sight H 2 O column densities of ∼4 × 10 13 cm −2 near the equatorial plane, with a ∼50 000 km vertical scale height. The water torus appears to be rotationally cold (e.g. an excitation temperature of 16 K is measured for the 1113 GHz line) but dynamically excited, with non-Keplerian dispersion velocities of ∼2 km s −1 , and appears to be largely shaped by molecular collisions. From estimates of the influx rates of torus material into Saturn and Titan, we infer that Enceladus' activity is likely to be the ultimate source of water in the upper atmosphere of Saturn, but not in Titan's.

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“…On the other hand, space-based observatories such as ISO (Kessler et al 1996) and Herschel (Pilbratt et al 2010) have access to the mid-to far-infrared rotational (R-branch) lines of HD (Ulivi et al 1991, see also Table 2). While the Voyager/IRIS instrument could not detect these lines because of its insufficient spectral resolution, observations by the medium-to-high resolution spectrometers ISO-SWS (de Graauw et al 1996) and ISO-LWS (Clegg et al 1996) resulted in D/H values with significantly improved precision for all four giant planets (Griffin et al 1996;Encrenaz et al 1996;Feuchtgruber et al 1999;Lellouch et al 2001). The baseline spectral response calibration of the ISO-LWS instrument was obtained from Uranus observations.…”

Section: Introductionmentioning

confidence: 99%

The D/H ratio in the atmospheres of Uranus and Neptune fromHerschel-PACS observations

Feuchtgruber¹,

Lellouch²,

Orton³

et al. 2013

A&A

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Herschel-PACS measurements of the rotational R(0) and R(1) HD lines in the atmospheres of Uranus and Neptune are analyzed to derive a D/H ratio with improved precision for the two planets. The derivation of the D/H ratio also includes previous measurements of the R(2) line with the Short Wavelength Spectrometer on board the Infrared Space Observatory (ISO). The available spectroscopic line information of the three rotational transitions is discussed and applied in the radiative transfer calculations. The best simultaneous fit of all three lines requires only a minor departure from the Spitzer temperature profile of Uranus and a departure limited to 2K from the Voyager temperature profile of Neptune (each time around the tropopause). The resulting and remarkably similar D/H ratios for Uranus and Neptune are found to be (4.4 ± 0.4) × 10 −5 and (4.1 ± 0.4) × 10 −5 , respectively. Although the deuterium enrichment in the two atmospheres compared to the protosolar value is confirmed, it is found to be lower compared to previous analyses. Using interior models from the literature and assuming that complete mixing of the atmosphere and interior occured during the planets' history, we derive a D/H in protoplanetary ices between (5.75-7.0) × 10 −5 for Uranus and between (5.1-7.7) × 10 −5 for Neptune. Conversely, adopting a cometary D/H for the protoplanetary ices between (15-30) × 10 −5 , we constrain the interior models of the two planets to have an ice mass fraction of 14-32%, i.e., the two planets are rock-dominated.

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External supply of oxygen to the atmospheres of the giant planets

Cited by 223 publications

References 30 publications

Revisiting the solid HDO/H$_\mathsf{2}$O abundances

Revisiting the solid HDO/H$_\mathsf{2}$O abundances

Direct detection of the Enceladus water torus withHerschel

The D/H ratio in the atmospheres of Uranus and Neptune fromHerschel-PACS observations

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