Saturn's cloud structure and temporal evolution from ten years of Hubble Space Telescope images (1994–2003)

Pérez‐Hoyos, S.; Sánchez‐Lavega, A.; French, R. G.; Rojas, J. F.

doi:10.1016/j.icarus.2005.01.014

Cited by 83 publications

(127 citation statements)

References 42 publications

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“…Long-term changes, probably coupled to the seasonal insolation cycle, were also detected in the haze optical depth above the ammonia cloud deck from a 1967-1984 spectroscopic survey performed by Trafton (1985). This variability study was extended later from 1986 to 1989 by Karkoschka and Tomasko (1992) using ground-based data and from 1994 to 2003 by Pérez-Hoyos et al (2005) and Karkoschka and Tomasko (2005) using HST images.…”

Section: Saturn Science Between the Voyager And Cassini Epochsmentioning

confidence: 75%

“…(3) While the jet profile is stable in its latitudinal location on Saturn (Smith et al 1981;Sánchez-Lavega et al 2000, the cloud/haze bands change their brightness and edge positions on time scales of both years (Sánchez-Lavega et al 1993a;Pérez-Hoyos et al 2005;Karkoschka and Tomasko 2005) and months (Sánchez-Lavega et al 1993a;Pérez-Hoyos et al 2006). The brightness changes are wavelength dependent.…”

Section: Albedo Patterns Vs Jets On Saturn Vs Jupitermentioning

confidence: 99%

“…The dragon storm is not visible in the UV3 (338 nm) and MT3 filters (Dyudina et al 2007). Using HST multi-wavelength images and a radiative transfer model, Pérez-Hoyos et al (2005) put the convective cloud tops at ~200 mbar. If the coincident appearance of SEDs and the dragon storm is evidence of lightning, it implies that the westward jets in which the Voyager and Cassini events occurred have lapse rates significantly in excess of the moist adiabatic lapse rate at depth, as is the case for lightning-producing convection on Earth.…”

Section: Convective Clouds and Lightningmentioning

confidence: 99%

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Saturn Atmospheric Structure and Dynamics

Genio

Achterberg

Baines

et al. 2009

Saturn From Cassini-Huygens

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Section: Saturn Science Between the Voyager And Cassini Epochsmentioning

confidence: 75%

Section: Albedo Patterns Vs Jets On Saturn Vs Jupitermentioning

confidence: 99%

Section: Convective Clouds and Lightningmentioning

confidence: 99%

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Saturn Atmospheric Structure and Dynamics

Genio

Achterberg

Baines

et al. 2009

Saturn From Cassini-Huygens

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“…Finally, the 430 nm images (blue) present the highest contrast corresponding to intermediate levels. Details on the Cassini filters can be found in Porco et al (2004) and for the HST filters in Pérez-Hoyos et al (2005), and references therein. Both sets of filters are compared in Sánchez-Lavega et al (2006).…”

Section: Observationsmentioning

confidence: 99%

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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“…Although there are many works dealing with calibrated observations in the visible part of the spectrum for Jupiter and Saturn, including Hubble Space Telescope (HST) calibrated ob- Tables A1-A4 and B1-B8 are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/ servations (Pérez-Hoyos et al 2005;Karkoschka & Tomasko 2005) or spacecraft imaging ) and ground-based multispectral photometry (Mallama et al 2017), the near-infrared side of the spectrum (SWIR; short wavelength infrared) has been analyzed less often (Clark & McCord 1979;de Pater et al 2010). This part of the spectrum is of particular interest to prepare for James Webb Space Telescope (JWST) image observations with the NIRCAM instrument of Jupiter to Neptune since JWST will achieve a spatial resolution better than Hubble Space Telescope (HST) from 0.7 to 2.1 microns (Norwood et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Temporal and spatial variations of the absolute reflectivity of Jupiter and Saturn from 0.38 to 1.7μm with PlanetCam-UPV/EHU

Mendikoa¹,

Sánchez‐Lavega²,

Pérez‐Hoyos³

et al. 2017

A&A

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Aims. We provide measurements of the absolute reflectivity of Jupiter and Saturn along their central meridians in filters covering a wide range of visible and near-infrared wavelengths (from 0.38 to 1.7 µm) that are not often presented in the literature. We also give measurements of the geometric albedo of both planets and discuss the limb-darkening behavior and temporal variability of their reflectivity values for a period of four years (2012)(2013)(2014)(2015)(2016).Methods. This work is based on observations with the PlanetCam-UPV/EHU instrument at the 1.23 m and 2.2 m telescopes in Calar Alto Observatory (Spain). The instrument simultaneously observes in two channels: visible (VIS; 0.38-1.0 µm) and short-wave infrared (SWIR; 1.0-1.7 µm). We obtained high-resolution observations via the lucky-imaging method. Results. We show that our calibration is consistent with previous independent determinations of reflectivity values of these planets and, for future reference, provide new data extended in the wavelength range and in the time. Our results have an uncertainty in absolute calibration of 10-20%. We show that under the hypothesis of constant geometric albedo, we are able to detect absolute reflectivity changes related to planetary temporal evolution of about 5-10%.

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Saturn's cloud structure and temporal evolution from ten years of Hubble Space Telescope images (1994–2003)

Cited by 83 publications

References 42 publications

Saturn Atmospheric Structure and Dynamics

Saturn Atmospheric Structure and Dynamics

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

Temporal and spatial variations of the absolute reflectivity of Jupiter and Saturn from 0.38 to 1.7μm with PlanetCam-UPV/EHU

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