The tropospheric gas composition of Jupiter's north equatorial belt /NH3, PH3, CH3D, GeH4, H2O/ and the Jovian D/H isotopic ratio

Kunde, V. G.; Hanel, Reinhold; Maguire, W. C.; Gautier, D.; Baluteau, J. P.; Marten, A.; Chédin, A.; Husson, N.; Scott, N. A.

doi:10.1086/160516

Cited by 219 publications

(108 citation statements)

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“…1) using the Jovian temperature proÐle from V oyager (Lindal et al 1981), the relation for vapor pressure given in Appendix A, and a subcloud mole fraction of 3 ] 10~5 (a wide range of abundances below the expected base of the Jovian ammonia cloud have been reported ; we adopt the value at 0.6 bars retrieved by Kunde et al [1982] for the Northern Equatorial Belt, which also agrees with the best-Ðt values of Carlson, Lacis, & Rossow [1993] and Brooke et al [1998]). The cloud base appears at 0.42 bars, where the temperature is 129 K. Although absent in the Ðgures of Lewis (1969 ; likely caused by reduced vertical resolution), in our interpretation of that model, the vapor is not entirely depleted in the lowest reaches of the cloud (where hence, increases above the cloud q c \ q t ) ; q c base.…”

Section: Previous Modelsmentioning

confidence: 52%

Precipitating Condensation Clouds in Substellar Atmospheres

Ackerman

Marley

2001

ApJ

756

1,283

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We present a method to calculate vertical proÐles of particle size distributions in condensation clouds of giant planets and brown dwarfs. The method assumes a balance between turbulent di †usion and sedimentation in horizontally uniform cloud decks. Calculations for the Jovian ammonia cloud are compared with results from previous methods. An adjustable parameter describing the efficiency of sedimentation allows the new model to span the range of predictions made by previous models. Calculations for the Jovian ammonia cloud are consistent with observations. Example calculations are provided for water, silicate, and iron clouds on brown dwarfs and on a cool extrasolar giant planet. We Ðnd that precipitating cloud decks naturally account for the characteristic trends seen in the spectra of Land T-type ultracool dwarfs.

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Section: Previous Modelsmentioning

confidence: 52%

Precipitating Condensation Clouds in Substellar Atmospheres

Ackerman

Marley

2001

ApJ

756

1,283

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“…It was known from remote sensing observations that the atmosphere above the tropopause, about the 150 mbar level (260 mbar in the 5-/xm hot spot), is stably stratified [Kunde et al, 1982;Eshleman et al, 1979] Ioannou and Lindzen [1994] suggested, the interior heat flux of Jupiter might then be carried out in a number of isolated thermal plumes, rather than by a global-scale convective pattern, and the driving mechanism for the zonal winds might be the gravitational tides rather than solar and internal heating [Ioannou and Lindzen, 1994]. One of the primary objectives of the ASI experiment was to determine the static stability of the atmosphere over the entire range of heights for which temperature was either directly measured during probe descent, or inferred from probe accelerations during entry.…”

Section: Static Stabilitymentioning

confidence: 99%

Thermal structure of Jupiter's atmosphere near the edge of a 5‐μm hot spot in the north equatorial belt

Seiff¹,

Kirk²,

Knight³

et al. 1998

J. Geophys. Res.

327

286

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Abstract. Thermal structure of the atmosphere of Jupiter was measured from 1029 km above to 133 km below the 1-bar level during entry and descent of the Galileo probe. The data confirm the hot exosphere observed by Voyager (---900 K at 1 nanobar). The deep atmosphere, which reached 429 K at 22 bars, was close to dry adiabatic from 6 to 16 bars within an uncertainty ---0.1 K/km. The upper atmosphere was dominated by gravity waves from the tropopause to the exosphere. Shorter waves were fully absorbed below 300 km, while longer wave amplitudes first grew, then were damped at the higher altitudes. A remarkably deep isothermal layer was found in the stratosphere from 90 to 290 km with T ---160 K. Just above the tropopause at 260 mbar, there was a second isothermal region ---25 km deep with T ---112 K. Between 10 and 1000 mbar, the data substantially agree with Voyager radio occultations. The Voyager 1 equatorial occultation was similar in detail to the present sounding through the tropopause region. The Voyager IRIS average thermal structure in the north equatorial belt (NEB) approximates a smoothed fit to the present data between 0.03 and 400 mbar. Differences are partly a result of large differences in vertical resolution but may also reflect differences between a hot spot and the average NEB. At 15 < p < 22 bars, where it was necessary to extrapolate the pressure calibration to sensor temperatures up to 118øC, the data indicate a stable layer in which stability increases with depth. Consistent with the indication of stability, regular fluctuations in probe vertical velocity imply gravity waves in this layer. At p > 4 bars, probe descent velocities derived from the data are consistently unsteady, suggesting the presence of large-scale turbulence or gravity waves. However, there was no evidence of turbulent temperature fluctuations >0.12 K. A conspicuous pause in the rate of decrease of descent velocity between 1.1 and 1.35 bars, where a disturbance was also detected by the two radio Doppler experiments, implies strong vertical flow in the cloud seen by the probe nephelometer. At p < 0.6 bar, measured temperatures were ---3 K warmer than the dry adiabat, possible evidence of radiative warming. This could be associated with a tenuous cloud detected by the probe nephelometer above the 0.51 bar level. For an ammonia cloud to form at this level, the required abundance is ---0.20 x solar. IntroductionThis paper reports principal results of the Galileo probe atmosphere structure experiment. The primary goal of the experiment was to define the thermal structure of Jupiter's atmosphere below the clouds, a region inaccessible to remote sensing, by direct sensing of atmospheric temperature and , 1996]. It was our intent to obtain measurements through and well below the clouds, to improve accuracy and resolution, and so to define the atmospheric stability against overturning, observe thermal effects of clouds, detect and quantify turbulence, and make other dynamical observations.Densities at a few levels in the upper atmosp...

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“…Since the region observed by the RT spectra was similar to that encountered by the Galileo entry probe, the temperature/pressure profile was assumed to be that returned by the probe [Seiff et al, 1996]. The mean a priori composition was then set to that shown in Table 1 and is based upon the probe mass spectrometer results [Niemann et al, 1996] and previous studies of the Voyager infrared imaging spectrometer (IRIS) data such as Kunde et al [1982], Carlson et al [1993], and other sources listed in the table. The atmosphere was split at pressures below 11 bars into 20 layers of equal path length, found to be the best compromise between speed and error by comparison with a precision line-by-line model using many layers (section 3.1.3).…”

Section: Forward Modelmentioning

confidence: 99%

Cloud structure and atmospheric composition of Jupiter retrieved from Galileo near‐infrared mapping spectrometer real‐time spectra

Irwin¹,

Weir²,

Smith³

et al. 1998

J. Geophys. Res.

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Abstract. The first four complete spectra recorded by the near infrared mapping spectrometer (NIMS) instrument on the Galileo spacecraft in 1996 have been analyzed. These spectra remain the only ones which have been obtained at maximum resolution over the entire NIMS wavelength range of 0.7 -5.2 gm. The spectra cover the edge of a "warm" spot at location 5øN, 85øW. We have analyzed the spectra first with reflecting layer models and then with full multiple scattering models using the method of correlated-k. We find that there is strong evidence for three different cloud layers composed of a haze consistent with 0.5-gm radius tholins at 0.2 bar, a cloud of 0.75-gm NH 3 particles at about 0.7 bar, and a two-component NH4SH cloud at about 1.4 bars with both 50.0-and 0.45-gm particles, the former being responsible for the main 5-gm cloud opacity. The NH 3 relative humidity above the cloud tops is found to decrease slightly as the 5-gm brightness increases, with a mean value of approximately 14%. We also find that the mean volume mixing ratio of ammonia above the middle (NH4SH) cloud deck is (1.7+0.1) x 10 -4 and shows a similar, though less discernible decrease with increasing 5-gm brightness. The deep volume mixing ratios of deuterated methane and phosphine are found to be constant and we estimate their mean values to be (4.9+0.2) x 10 -7 and (7.7+0.2) x 10 -7, respectively. The fractional scale height of phosphine above the 1 bar level is found to be 27.1+1.4% and shows a slight decrease with increasing 5-gm brightness. The relative humidity of water vapor is found to be approximately 7%, but while this and all the previous observations are consistent with the assumption that "hot spots" are regions of downwelling, desiccated air, we find that the water vapor relative humidity increases as the 5-gm brightness increases.

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The tropospheric gas composition of Jupiter's north equatorial belt /NH3, PH3, CH3D, GeH4, H2O/ and the Jovian D/H isotopic ratio

Cited by 219 publications

References 0 publications

Precipitating Condensation Clouds in Substellar Atmospheres

Precipitating Condensation Clouds in Substellar Atmospheres

Thermal structure of Jupiter's atmosphere near the edge of a 5‐μm hot spot in the north equatorial belt

Cloud structure and atmospheric composition of Jupiter retrieved from Galileo near‐infrared mapping spectrometer real‐time spectra

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