The visible bands of ammonia - Band strengths, curves of growth, and the spatial distribution of ammonia on Jupiter

Lutz, B. L.; Owen, T.

doi:10.1086/157632

Cited by 21 publications

(42 citation statements)

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“…Perhaps the method used by West et al to infer a continuum reference for the Voyager 619-nm images might have been somewhat biased by methane absorption present in the broadband filters used to establish the continuum. Groundbased measurements showing almost the same equivalent widths in the EZ and NEB (Lutz and Owen 1980), which seem to support the West et al result, might have missed the increase in dark spots because of their zonal averaging and low spatial resolution. It is interesting to compare our results with those of Gierasch et al (1986) who derived zonal mean optical depths at 2050 cm −1 (4.878 µm) and at 225 cm −1 (44.4 µm) from Voyager IRIS observations of Jupiter.…”

Section: Discussionsupporting

confidence: 72%

Jupiter's Cloud Structure as Constrained by Galileo Probe and HST Observations

Sromovsky¹,

Fry

2002

Icarus

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Section: Discussionsupporting

confidence: 72%

Jupiter's Cloud Structure as Constrained by Galileo Probe and HST Observations

Sromovsky¹,

Fry

2002

Icarus

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“…Figure 11 shows our best fit to the Equatorial Zone spectrum using the combined Bowles et al and Lutz&Owen data, and then the fit resulting from using the NH 3 k-table generated from the ExoMol-C2018 line list . Figure 12 shows the same comparison for a spectrum measured in the North Equatorial Belt (corresponding to Fig. As can be seen we are able to fit the VLT/MUSE observations of the EZ and NEB significantly better with the ExoMol-C2018 NH 3 absorption data than we can using our previous best combination of the data of Bowles et al (2008) and Lutz and Owen (1980).…”

Section: Analysis Of Muse Observationsmentioning

confidence: 52%

“…In Fig. 1 of Lutz and Owen (1980), the shorter wavelength absorption peak is clearly at a wavelength less than 5500Å and the second peak at a wavelength least 25Å longer. However, in their Fig.…”

Section: Comparison Withmentioning

confidence: 91%

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Analysis of gaseous ammonia (NH3) absorption in the visible spectrum of Jupiter - Update

Irwin

Bowles

Braude

et al. 2019

Icarus

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An analysis of currently available ammonia (NH 3 ) visible-to-near-infrared gas absorption data was recently undertaken by Irwin et al. (Icarus, 302 (2018) 426) to help interpret Very Large Telescope (VLT) MUSE observations of Jupiter from 0.48 -0.93 µm, made in support of the NASA/Juno mission. Since this analysis a newly revised set of ammonia line data, covering the previously poorly constrained range 0.5 -0.833 µm, has been released by the ExoMol project, "C2018" , which demonstrates significant advantages over previously available data sets, and providing for the first time complete line data for the previously poorly constrained 5520-and 6475-Å bands of NH 3 . In this paper we compare spectra calculated using the ExoMol-C2018 data set with spectra calculated from previous sources to demonstrate its advantages. We conclude that at the present time the ExoMol-C2018 dataset provides the most reliable ammonia absorption source for analysing low-to medium-resolution spectra of Jupiter in the visible/near-IR spectral range, but note that the data are less able to model high-resolution spectra owing to small, but significant inaccuracies in the line wavenumber estimates. This work is of significance not only for solar system planetary physics, but for future proposed observations of Jupiter-like planets orbiting other stars, such as with NASA's planned Wide-Field Infrared Survey Telescope (WFIRST). Subject headings: planets and satellites: atmospheres -planets and satellites: individual (Jupiter) Yurchenko 2012; Tennyson et al. 2016). The new line list covers an extended wavelength

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“…A total of eleven terms were used in the cosine expansion of the intensities. To compute the equivalent widths of the absorption bands, we used the absorption coefficients of Giver (1978) and Lutz and Owen (1980) for methane and ammonia, respectively. We included the methane absorption in the computation of the NH3-6450 band profile.…”

Section: Analysis Of the Observations And Discussionmentioning

confidence: 99%

Spatially resolved spectroscopic observations of Jupiter during the 1987 opposition

Moreno

Molina

1989

Earth Moon Planet

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Spectroscopic observations in the spectral region AA 6000--6600 ~, of major belts and zones of Jupiter have been carded out at Calar Alto Observatory (Spain) during the 1987 opposition, in support to the International Jupiter Watch Program. More than a hundred long-slit, medium resolution spectra have been taken at the coud6 focus of the 1.52 m telescope. The longitudinal and latitudinal distribution of the equivalent widths of the methane and ammonia absorption bands at 6190A and 6450A have been investigated. Unlike the CH4-6190~, band, the longitudinal distribution in the NH~-6450 ,~ band shows asymmetries in some of the Jovian regions analyzed, being the absorption greater at West than at East limbs. These results are interpreted in terms of inhomogeneous scattering models by the simultaneous variation of the NH3 cloud optical thickness and its altitude level. The north--south scans show little latitudinal dependence on absorption in both methane and ammonia bands, although some relationship could be established between the absorption and relative continuum refleetivity variation.Resnmen. Se presentan los resultados obtenidos de las observaciones espectrosc6picas de las principales zonas y cinturones de Jfipiter realizadas durante la oposici6n de 1987 como una contribuci6n al International Jupiter Watch Program. Las observaciones fueron Ilevadas a cabo haciendo uso del foco coud6 del telescopio de 1.52 m del observatorio hispanoalem~n de Calar Alto (Espafia), habi6ndose obtenido algo mils de cien espectros, de resoluci6n media, en la regi6n espectral de 6000-6600 ,~. Se exponen los resultados de las anchuras equivalentes de Ins bandas de absorci6n del metano en 6190A, y del amoniaco en 6450 A,, estudi~ndose, al mismo tiempo, la distribuci6n tanto longitudinal como latitudinal de las mismas. Mientras que los resultados para ia banda del metano presentan un comportamiento sim6trico en todas ias regiones analizadas, las anchuras equivalentes para la banda NH3-6450 A presentan un comportamiento asim6trico en algunas regiones del planeta, con una mayor absorci6n hacia el limbo del oeste que hacia el del este. Los resultados son interpretados en base aun modelo de 'scattering' no homog6neo, variando, simultfineamente, el espesor 6ptico y la altitud de la nube de amoniaco. Los espectros tornados en la direcci6n norte-sur, aunque presentan una dependencia latitudinal pequefia en la absorci6n de las bandas mencionadas, sugieren una relaci6n entre la absorci6n y las variaciones de reflectividad en el continuo.

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The visible bands of ammonia - Band strengths, curves of growth, and the spatial distribution of ammonia on Jupiter

Cited by 21 publications

References 0 publications

Jupiter's Cloud Structure as Constrained by Galileo Probe and HST Observations

Jupiter's Cloud Structure as Constrained by Galileo Probe and HST Observations

Analysis of gaseous ammonia (NH3) absorption in the visible spectrum of Jupiter - Update

Spatially resolved spectroscopic observations of Jupiter during the 1987 opposition

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