Jupiter's Tropospheric Thermal Emission. II. Power Spectrum Analysis and Wave Search

Harrington, J.; Dowling, T. E.; Baron, R. L.

doi:10.1006/icar.1996.0188

Cited by 25 publications

(38 citation statements)

References 8 publications

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“…We also interpret the results in terms of Rossby waves and discuss their implications on vertical structure. Previous works that point out wave propagation closely related to our study were presented very recently by Harrington et al [1996b] and Deming et al [1997].…”

Section: Introductionsupporting

confidence: 73%

Evolution and persistence of 5‐μm hot spots at the Galileo probe entry latitude

Ortiz¹,

Orton²,

Friedson³

et al. 1998

J. Geophys. Res.

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Abstract. We present a study on the longitudinal locations, morphology, and evolution of the 5-/xm hot spots at 6.5øN latitude (planetocentric) from an extensive Infrared Telescope Facility-National Science Foundation Camera (IRTF-NSFCAM) data set spanning more than 3 years, which includes the date of the Galileo probe entry. A probabilistic analysis of the data shows that within periods of several months to even more than a year, there are eight or nine longitudinal areas with high likelihood of containing a 5-/xm hot spot. These areas drift together with respect to System III at a rate which changes only slowly in time, and they are quasi evenly spaced, suggesting a wave feature. A spectral analysis of the radiance data reveals that planetary wavenumbers 8, 9, and 10 are predominant in the data, 10 having more spectral power in several time periods when the speed was 103.5-102.5 m/s, while planetary wavenumber 8 has much more power when the speed is (99.5 _+ 0.5) m/s. By using the Galileo probe zonal wind speed [Atkinson et al., 1997] at the level of the main cloud that is opaque to the radiation at 5/xm (-2 bar), our drift corrections imply a westward phase speed for the proposed wave. The wavenumbers and phase speeds are found to be consistent with an equatorial Rossby wave, and the dispersive properties of this wave can account for the observed simultaneous changes in the dominant wavenumber and drift speed. We take advantage of this interpretation to infer properties of the vertical structure at 6.5øN.

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Section: Introductionsupporting

confidence: 73%

Evolution and persistence of 5‐μm hot spots at the Galileo probe entry latitude

Ortiz¹,

Orton²,

Friedson³

et al. 1998

J. Geophys. Res.

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“…Jupiter's results for larger scales range from n 1 ~ -0.7 (Harrington et al 1996b) to n 1 ~ -1.3 (this work). On the other hand, results for smaller scales range from n 2 ~ -2.5 (this work, excluding UV results to be commented later) to n 2 ~ -3.0 (Mitchell 1982).…”

Section: Discussion Of the Zonal Power Spectra And Conclusionmentioning

confidence: 63%

“…3; see also Harrington et al 1996b). Those ranges are separated by a turning point at wavenumber k I .…”

Section: Accepted M Manuscriptmentioning

confidence: 85%

“…For jets between 40ºN and 40ºS they found the slope shown in Table 5 with the turning-point assumed to be located at k = 10. On the other hand, Harrington et al (1996b) studied the power spectra of Jupiter's cloud opacity spatial distribution at 5 µm. At this wavelength, the radiation coming from the interior of the planet is blocked by clouds somewhere between 2 and 5 bars pressure levels so they retrieved the power spectra of a deeper cloud.…”

Section: Discussion Of the Zonal Power Spectra And Conclusionmentioning

confidence: 99%

“…One strategy to characterize the global cloud patterns in planetary atmospheres is the analysis at different wavelengths of the cloud field brightness, as Travis (1978) did for the case of Earth and Venus, Peralta et al (2007) for Venus and Harrington et al (1996aand Harrington et al ( , 1996b for Jupiter. The brightness structure is important for two reasons.…”

Section: Introductionmentioning

confidence: 99%

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Brightness power spectral distribution and waves in Jupiter's upper cloud and hazes

Barrado-Izagirre

Pérez‐Hoyos

Sánchez‐Lavega

2009

Icarus

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To cite this version:N. Barrado-Izagirre, S. Pérez-Hoyos, A. Sánchez-Lavega. Brightness power spectral distribution and waves in Jupiter's upper cloud and hazes. Icarus, Elsevier, 2009, 202 (1) This is a PDF file of an unedited manuscript that has been accepted for publication. As a service to our customers we are providing this early version of the manuscript. The manuscript will undergo copyediting, typesetting, and review of the resulting proof before it is published in its final form. Please note that during the production process errors may be discovered which could affect the content, and all legal disclaimers that apply to the journal pertain. infrared and blue wavelengths, average spectral slopes are n 1 = -1.3 ± 0.4 for shorter wavenumbers (k < 80), and n 2 = -2.5 ± 0.7 for greater wavenumbers, whereas for the ultraviolet n 1 = -1.9 ± 0.4 and n 2 = -0.7 ± 0.4, possibly showing a different dynamical regime. We find a turning point in the spectra between both regimes at wavenumber k ~ 80 (corresponding to L ~ 1000 km) for all wavelengths.

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