A new model of the hydrogen and helium-broadened microwave opacity of ammonia based on extensive laboratory measurements

Hanley, Thomas R.; Steffes, Paul G.; Karpowicz, Bryan M.

doi:10.1016/j.icarus.2009.02.002

Cited by 39 publications

(38 citation statements)

References 51 publications

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“…MWR retrievals were not made from latitudes poleward of 40° from the equator to avoid interference from synchrotron radiation. Results from the Galileo Probe relay attenuation signal experiment at this pressure [ Folkner et al , ; Hanley et al , ] are shown by the open diamond and associated uncertainties.…”

Section: Resultsmentioning

confidence: 99%

Multiple‐wavelength sensing of Jupiter during the Juno mission's first perijove passage

Orton

Momary

Ingersoll

et al. 2017

Geophysical Research Letters

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We compare Jupiter observations made around 27 August 2016 by Juno's JunoCam, Jovian Infrared Auroral Mapper (JIRAM), MicroWave Radiometer (MWR) instruments, and NASA's Infrared Telescope Facility. Visibly dark regions are highly correlated with bright areas at 5 µm, a wavelength sensitive to gaseous NH3 gas and particulate opacity at p ≤5 bars. A general correlation between 5‐µm and microwave radiances arises from a similar dependence on NH3 opacity. Significant exceptions are present and probably arise from additional particulate opacity at 5 µm. JIRAM spectroscopy and the MWR derive consistent 5‐bar NH3 abundances that are within the lower bounds of Galileo measurement uncertainties. Vigorous upward vertical transport near the equator is likely responsible for high NH3 abundances and with enhanced abundances of some disequilibrium species used as indirect indicators of vertical motions.

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Section: Resultsmentioning

confidence: 99%

Multiple‐wavelength sensing of Jupiter during the Juno mission's first perijove passage

Orton

Momary

Ingersoll

et al. 2017

Geophysical Research Letters

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“…The parameters are the same as those used to fit the spectrum at 2144 cm −1 except for H 2 O and NH 3 . We initially used a vertical profile of NH 3 derived from absorption of the radio signal from the Galileo Probe (Folkner et al 1998 as modified by Hanley et al 2009). We found that a scaling factor of 2 was required to fit the NH 3 absorption features shown in Figure 7.…”

Section: Data Analysis and Resultsmentioning

confidence: 99%

Jupiter’s Deep Cloud Structure Revealed Using Keck Observations of Spectrally Resolved Line Shapes

Bjoraker

Wong

Pater

et al. 2015

ApJ

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Technique: We present a method to determine the pressure at which significant cloud opacity is present between 2 and 6 bars on Jupiter. We use (a) the strength of a Fraunhofer absorption line in a zone to determine the ratio of reflected sunlight to thermal emission, and (b) pressure-broadened line profiles of deuterated methane (CH 3 D) at 4.66 μm to determine the location of clouds. We use radiative transfer models to constrain the altitude region of both the solar and thermal components of Jupiter's 5 μm spectrum. Results: For nearly all latitudes on Jupiter the thermal component is large enough to constrain the deep cloud structure even when upper clouds are present. We find that hot spots, belts, and high latitudes have broader line profiles than do zones. Radiative transfer models show that hot spots in the North Equatorial Belt and South Equatorial Belt (SEB) typically do not have opaque clouds at pressures greater than 2 bars. The South Tropical Zone (STZ) at 32S has an opaque cloud top between 4 and 5 bars. From thermochemical models this must be a water cloud. We measured the variation of the equivalent width of CH 3 D with latitude for comparison with Jupiter's belt-zone structure. We also constrained the vertical profile of H 2 O in an SEB hot spot and in the STZ. The hot spot is very dry for P < 4.5 bars and then follows the H 2 O profile observed by the Galileo Probe. The STZ has a saturated H 2 O profile above its cloud top between 4 and 5 bars.

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“…Combined with a model of the atmosphere, JAMRT computes radiances from profiles of temperature, ammonia and water from the cloud tops down to pressures of 1000 bars. The model uses experimental data on the opacity of ammonia and water in hydrogen-helium mixtures at temperatures up to 600 K and pressures up to 100 bars (18,(41)(42)(43). The uncertainties of the opacity models have been determined to be about 5% to 7% from low pressures up to 100 bars.…”

Section: Microwave Radiometermentioning

confidence: 99%

Jupiter’s interior and deep atmosphere: The initial pole-to-pole passes with the Juno spacecraft

Bolton

Adriani

Adumitroaie

et al. 2017

Science

272

237

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Juno swoops around giant Jupiter Jupiter is the largest and most massive planet in our solar system. NASA's Juno spacecraft arrived at Jupiter on 4 July 2016 and made its first close pass on 27 August 2016. Bolton et al. present results from Juno's flight just above the cloud tops, including images of weather in the polar regions and measurements of the magnetic and gravitational fields. Juno also used microwaves to peer below the visible surface, spotting gas welling up from the deep interior. Connerney et al. measured Jupiter's aurorae and plasma environment, both as Juno approached the planet and during its first close orbit. Science , this issue p. 821 , p. 826

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A new model of the hydrogen and helium-broadened microwave opacity of ammonia based on extensive laboratory measurements

Cited by 39 publications

References 51 publications

Multiple‐wavelength sensing of Jupiter during the Juno mission's first perijove passage

Multiple‐wavelength sensing of Jupiter during the Juno mission's first perijove passage

Jupiter’s Deep Cloud Structure Revealed Using Keck Observations of Spectrally Resolved Line Shapes

Jupiter’s interior and deep atmosphere: The initial pole-to-pole passes with the Juno spacecraft

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