Jupiter's polar clouds and waves from Cassini and HST images: 1993–2006

Barrado-Izagirre, N.; Sánchez‐Lavega, A.; Pérez‐Hoyos, S.; Hueso, R.

doi:10.1016/j.icarus.2007.08.025

Cited by 34 publications

(36 citation statements)

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“…HST images were pipeline preprocessed and calibrated and Cassini ISS ones were photometrically calibrated with CISSCAL software (Porco et al 2004). We used LAIA software (Cano, 1998; see e. g. García-Melendo and Sánchez-Lavega, 2001 for details) for HST image navigation and projection; whereas for Cassini images PLIA software was employed (Hueso et al 2008). Both use parts of the VICAR code for pixel to longitude-latitude coordinates transformation (Barrey 1984).…”

Section: [Table 1]mentioning

confidence: 99%

“…Some examples are, the Great Red Spot wake (westward), the cyclonic filamentary regions (Mitchell 1982) or others that sporadically form when large scale disturbances occur, as during the South Equatorial Belt events (Sánchez-Lavega and Gomez 1996) or the North Temperate Belt disturbances (e.g. see Sánchez-Lavega et al 2008). In fact, Jupiter's visible clouds represent a privileged site for the study of chaotic and turbulent cloud patterns.…”

Section: Introductionmentioning

confidence: 99%

“…1c) are flat and homogeneous in albedo and therefore show less wave activity. However, some striking features arise at the ultraviolet maps, as for example, the polar wave at 57ºS in 1995 and 2000 (Vincent et al 2000;Barrado-Izagirre et al 2008). Particularly interesting is the wave patchy train at 15ºN observed during the Cassini period (discovery by Li et al 2006b) that was not present, however, in the HST maps.…”

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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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Section: [Table 1]mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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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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“…The software has been successfully validated in studies of Galileo SSI images of Venus (Peralta et al, 2007a,b), Cassini ISS images of Jupiter (Barrado-Izagirre et al, 2008;Hueso et al, 2009) and Saturn (Sánchez-Lavega et al, 2007del Río-Gaztelurrutia et al, 2010), New Horizons LORRI images of Jupiter (Hueso et al, 2009) and Venus Express VIRTIS-M hyperspectral image cubes of Venus Sánchez-Lavega et al, 2008).…”

Section: Discussionmentioning

confidence: 99%

The Planetary Laboratory for Image Analysis (PLIA)

Hueso

Legarreta

Rojas

et al. 2010

Advances in Space Research

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“…Gravity waves at cloud level travelling in the westward direction with wavelengths of about 300 km have been reported by different studies Article published by EDP Sciences (Flasar & Gierasch 1986;Reuter et al 2007;Arregi et al 2009). As stated above, large scale waves in the cloud field, pressumably of Rossby type, have been identified and studied by different teams (Allison 1990;Ortiz et al 1998;Arregi et al 2006;Li et al 2006;Barrado-Izagirre et al 2008;García-Melendo et al 2011;Choi et al 2013). Finally equatorial waves in the temperature field have been detected with wavenumbers in the range 1−11 (Deming et al 1997).…”

Section: Introductionmentioning

confidence: 91%

A large active wave trapped in Jupiter’s equator

Legarreta

Barrado-Izagirre

García-Melendo

et al. 2016

A&A

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Context. A peculiar atmospheric feature was observed in the equatorial zone (EZ) of Jupiter between September and December 2012 in ground-based and Hubble Space Telescope (HST) images. This feature consisted of two low albedo Y-shaped cloud structures (Y1 and Y2) oriented along the equator and centred on it (latitude 0.5• −1 • N). Aims. We wanted to characterize these features, and also tried to find out their properties and understand their nature. Methods. We tracked these features to obtain their velocity and analyse their cloud morphology and the interaction with their surroundings. We present numerical simulations of the phenomenon based on one-and two-layer shallow water models under a Gaussian pulse excitation. Results. Each Y feature had a characteristic zonal length of ∼15• (18 000 km) and a meridional width (distance between the northsouth extremes of the Y) of 5• (6000 km), and moved eastward with a speed of around 20−40 m s −1 relative to Jupiter's mean flow. Their lifetime was 90 and 60 days for Y1 and Y2, respectively. In November, both Y1 and Y2 exhibited outbursts of rapidly evolving bright spots emerging from the Y vertex. The Y features were not visible at wavelengths of 255 or 890 nm, which suggests that they were vertically shallow and placed in altitude between the upper equatorial hazes and the main cloud deck. Numerical simulations of the dynamics of the Jovian equatorial region generate Kelvin and Rossby waves, which are similar to those in the Matsuno-Gill model for Earth's equatorial dynamics, and reproduce the observed cloud morphology and the main properties the main properties of the Y features.

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Jupiter's polar clouds and waves from Cassini and HST images: 1993–2006

Cited by 34 publications

References 34 publications

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

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

The Planetary Laboratory for Image Analysis (PLIA)

A large active wave trapped in Jupiter’s equator

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