Updated Galileo probe mass spectrometer measurements of carbon, oxygen, nitrogen, and sulfur on Jupiter

Wong, Michael H.; Mahaffy, P. R.; Atreya, S. K.; Niemann, H. B.; Owen, Tobias

doi:10.1016/j.icarus.2004.04.010

Cited by 323 publications

(329 citation statements)

References 59 publications

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“…Interestingly, however, the measured relative abundances are lower than would be predicted from the saturation vapor pressure data alone, suggesting that other processes, perhaps such as cloud condensation, are influencing the ability of spectroscopic observations to accurately estimate the water inventories of the giant planets. Galileo probe measurements of water vapor in the Jovian atmosphere (e.g., Wong et al, 2004) confirmed in general the dryer-than-expected nature of the upper troposphere, but the probe's entry into what appears to have been an anomalous "hot spot" complicates the extrapolation of the probe's measurements to the troposphere (and interior) overall.…”

Section: 2mentioning

confidence: 96%

Water on Planets

Bell

2009

Proc. IAU

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Abstract.Water is an abundant molecule in the Cosmos. It has exploitable and unique spectroscopic and physical properties and has been found to be ubiquitous in places that we would expect in the standard model of solar system formation and nebular condensation: beyond the snow line in outer solar system planets, moons, asteroids, and comets. However, water is also an important constituent of planetary bodies (dominating at least one of their surfaces) in the inner solar system, likely indicating significant mixing between inner and outer solar system reservoirs of water during planetary accretion and the early history of the solar system. Water has played a critical role in the differential evolution of the terrestrial planets Venus, Earth, and Mars, and the concept of the "habitable zone" where liquid water could be stable on an Earth-like planet provides a starting point for assessing the habitability of worlds in our solar system and beyond. Examples of potentially habitable environments outside this zone in our own solar system warn us that this concept should only be a guide, however-important exceptions will no doubt occur. Recent discoveries of past liquid water and abundant present subsurface ice on Mars, of water reservoirs in unexpected places like the poles of Mercury and the Moon and the subsurface of Enceladus, of water in circumstellar disks and in the atmospheres of extrasolar planets, and the expectation of the discovery of water on Earth-like worlds in the habitable zones around other stars make this an exciting time in the study of water on planets both in our own solar system, and beyond.

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Section: 2mentioning

confidence: 96%

Water on Planets

Bell

2009

Proc. IAU

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“…The value of H 2 O abundance reported for Jupiter corresponds to the deepest measurement made by the probe (at ∼ 20 bar). It is probably smaller than the planet's bulk water abundance, which remains unknown (Atreya et al 2003;Wong et al 2004;Mousis et al 2012). The He abundance in Jupiter has also been measured in situ by a JaminMascart interferometer (Helium Abundance Detector) aboard the Galileo probe (von Zahn and Hunten 1992;von Zahn et al 1998).…”

Section: Atmospheric Compositionmentioning

confidence: 99%

“…Elemental abundances have been expressed as a function of the protosolar abundances derived from Lodders et al (2009). The abundances of CH 4 , NH 3 , H 2 O, H 2 S, Ne, Ar, Kr and Xe were measured by the Galileo Probe Mass Spectrometer (GPMS) in Jupiter's atmosphere (Mahaffy et al 2000;Wong et al 2004). The value of H 2 O abundance reported for Jupiter corresponds to the deepest measurement made by the probe (at ∼ 20 bar).…”

Section: Atmospheric Compositionmentioning

confidence: 99%

“…PH 3 is the only species of our list of measurements in Jupiter whose abundance has been determined remotely by the Cassini Composite Infrared Spectrometer (CIRS) during the spacecraft encounter in 2000(Fletcher et al 2009a). The GPMS instrument aboard the Galileo probe has also performed the isotopic measurements presented for Jupiter in Table 3 (Niemann et al 1996Mahaffy et al 2000;Wong et al 2004). …”

Section: Atmospheric Compositionmentioning

confidence: 99%

“…Interestingly, the Galileo probe entry site in Jupiter's atmosphere was an unusually dry meteorological system. This implies that the probe did not measure the deep, well-mixed water abundance (Wong et al 2004). An interpretation of the volatile enrichments measured in the four giant planets is that their building blocks agglomerated from a mixture of rocks and crystalline ices that condensed during the cooling period of the protosolar nebula (Gautier et al 2001;Hersant et al 2004Hersant et al , 2008Alibert et al 2005aAlibert et al , 2005bGautier and Hersant 2005;Mousis et al 2006Mousis et al , 2009cMousis et al , 2012Marboeuf et al 2008Marboeuf et al , 2014aMarboeuf et al , 2014b.…”

Section: Interpretations Of the Volatile Enrichments In The Atmosphermentioning

confidence: 99%

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Constraints from Comets on the Formation and Volatile Acquisition of the Planets and Satellites

et al. 2015

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Comets play a dual role in understanding the formation and evolution of the solar system. First, the composition of comets provides information about the origin of the giant planets and their moons because comets formed early and their composition is not expected to have evolved significantly since formation. They, therefore serve as a record of conditions during the early stages of solar system formation. Once comets had formed, their orbits were perturbed allowing them to travel into the inner solar system and impact the planets. In this way they contributed to the volatile inventory of planetary atmospheres. We review here how knowledge of comet composition up to the time of the Rosetta mission has contributed to understanding the formation processes of the giant planets, their moons and small icy bodies in the solar system. We also discuss how comets contributed to the volatile inventories of the giant and terrestrial planets.

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Isotopes of nitrogen on Mars: Atmospheric measurements by Curiosity's mass spectrometer

Wong

Atreya

Mahaffy

et al. 2013

Geophysical Research Letters

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[1] The Sample Analysis at Mars (SAM) instrument suite on the Mars Science Laboratory (MSL) measured a Mars atmospheric14N/15N ratio of 173 ± 11 on sol 341 of the mission, agreeing with Viking's measurement of 168 ± 17. The MSL/SAM value was based on Quadrupole Mass Spectrometer measurements of an enriched atmospheric sample, with CO2 and H2O removed. Doubly ionized nitrogen data at m/z 14 and 14.5 had the highest signal/background ratio, with results confirmed by m/z 28 and 29 data. Gases in SNC meteorite glasses have been interpreted as mixtures containing a Martian atmospheric component, based partly on distinctive14N/15N and40Ar/14N ratios. Recent MSL/SAM measurements of the40Ar/14N ratio (0.51 ± 0.01) are incompatible with the Viking ratio (0.35 ± 0.08). The meteorite mixing line is more consistent with the atmospheric composition measured by Viking than by MSL.

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Updated Galileo probe mass spectrometer measurements of carbon, oxygen, nitrogen, and sulfur on Jupiter

Cited by 323 publications

References 59 publications

Water on Planets

Water on Planets

Constraints from Comets on the Formation and Volatile Acquisition of the Planets and Satellites

Isotopes of nitrogen on Mars: Atmospheric measurements by Curiosity's mass spectrometer

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