The 2009–2010 fade of Jupiter’s South Equatorial Belt: Vertical cloud structure models and zonal winds from visible imaging

Pérez‐Hoyos, S.; Sanz-Requena, J. F.; Barrado-Izagirre, N.; Rojas, J. F.; Sánchez‐Lavega, A.

doi:10.1016/j.icarus.2011.11.008

Cited by 39 publications

(58 citation statements)

References 43 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This is a reasonable result not only because of the smaller time difference between both profiles but also because of the visual appearance of the cloud morphology in both years. The appearance is very similar despite recent large-scale cyclic variations such as the Fade (2009−10) and Revival (2010) of the SEB (Pérez-Hoyos et al 2012;Fletcher et al 2011) or the impact of a 500 m object with Jupiter in 2009 at −55 • latitude (Sánchez-Lavega et al 2010), which resulted in a large dark debris cloud that moved at the same velocity as the general flow as retrieved from HST (Hammel et al 2010) and ground-based observations (Sánchez-Lavega et al 2011). The only notorious change between these two epochs occurred at latitude 27−28 • , where 2008 HST data showed a westward acceleration of the A74, page 8 of 11 jet (Asay-Davis et al 2011).…”

Section: Long-term Variationsmentioning

confidence: 77%

“…The mean intensity of the winds has shown temporal variability on the order of ∼10 ms −1 (Asay-Davis et al 2011) and a remarkable stability of the latitudes of the zonal jets' maximum velocities. Although some of the bands' morphology changes in periods of years (Peek 1958;Chapman & Reese 1968;Reese 1972;Minton 1972a,b;Smith & Hunt 1976;Sánchez-Lavega & Rodrigo 1985;Rogers 1995;Sánchez-Lavega & Gómez 1996;Sánchez-Lavega et al 1996;Fletcher et al 2011;Pérez-Hoyos et al 2012), the wind profile maintains a remarkable temporal stability. Furthermore, this zonal wind profile is not strongly affected by the dynamic perturbations at cloud level, such as those developed by convective storms like the South Equatorial Belt Disturbance (SEBD; Sánchez-Lavega et al 1996;Sánchez-Lavega & Gómez 1996) and the North Temperate Belt Disturbance (NTBD) (García-Melendo et al 2005Sánchez-Lavega et al 2008;Barrado-Izagirre et al 2009a).…”

Section: Introductionmentioning

confidence: 99%

“…Previous studies using these kinds of images , 2011aBarrado-Izagirre et al 2009a;Sánchez-Lavega et al 2008, 2011Pérez-Hoyos et al 2012) inferred wind velocities by manual tracking of long-lived cloud details, which had been tracked over many different images or image pairs separated by several planetary rotations. We show that an automatic cloud correlation technique such as those used to analyze higher resolution HST or spacecraft data also works for ground-based observations with small telescopes obtained by keen amateur observers.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Jupiter’s zonal winds and their variability studied with small-size telescopes

Barrado-Izagirre

Rojas

Hueso

et al. 2013

A&A

Self Cite

View full text Add to dashboard Cite

Context. The general circulation of Jupiter's atmosphere at cloud level is dominated by a system of zonal jets that alternate in direction with latitude. The winds, measured in high-resolution images obtained by different space missions and the Hubble Space Telescope, are overall stable in their latitude location with small changes in intensity at particular jets. However, the atmosphere experiences repetitive changes in the albedo of particular belts and zones that are subject to large-scale intense disturbances that may locally influence the profile. Aims. The lack of high-resolution images has not allowed the wind system to be studied with the regularity required to assess its stability with respect to these major changes or to other types of variations (e.g., seasonality). To amend that, we present a study of the zonal wind profile of Jupiter using images acquired around the 2011 opposition by a network of observers operating small-size telescopes with apertures in the range 0.20−1 m. Methods. Using an automatic correlation technique, we demonstrate the capability to extract the mean zonal winds in observing periods close to the opposition. A broad collaboration with skilled amateur astronomers opens the possibility to regularly study shortand long-term changes in the jets of Jupiter. Results. We compare the 2011 Jovian wind profile to those previously obtained. The winds did not experience significant short-term changes over 2011 but show noteworthy variations at particular latitudes when compared with wind profiles from previous years. Most of these variations are related to major changes in the cloud morphology of the planet, in particular at 7 • N where an intense eastward jet varies around 40 ms −1 in its intensity according to the development or not of the "dark projection" features, confirming previous results.

show abstract

Section: Long-term Variationsmentioning

confidence: 77%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Jupiter’s zonal winds and their variability studied with small-size telescopes

Barrado-Izagirre

Rojas

Hueso

et al. 2013

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…In this work, we profusely refer to a number of previous studies that served as an external reference for the absolute reflectivity values we obtain in this work. No seasonal variability has been reported in the atmosphere of Jupiter except for planetary-scale changes at particular belts and zones not linked to seasonal changes, (see Sánchez-Lavega et al 1996;Sánchez-Lavega et al 2008Fletcher et al 2011;Pérez-Hoyos et al 2012); however, Saturn is known to display hemispherical seasonal changes and changing viewing or illumination geometry owing to the tilt of its rotation axis (West et al 2009). For this reason, Saturn photometric values usually only serve as a snapshot for a particular season.…”

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

Self Cite

View full text Add to dashboard Cite

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%.

show abstract

“…Irregular and brusque variations caused by storms or structural changes in the planet's belts have also been observed in giant planets (e.g. Tejfel et al 1994;Sánchez-Lavega 1994;Rogers 2009;Fletcher et al 2011;Pérez-Hoyos et al 2012), and they are likely to happen in ultracool dwarfs as well. Photometric data from different epochs, separated by months, are already available for a few ultracool dwarfs (e.g.…”

Section: Introductionmentioning

confidence: 98%

Long-termKs-band photometric monitoring of L dwarfs

Martí¹,

Osorio²

2014

A&A

View full text Add to dashboard Cite

Context. Ultracool dwarfs ( < ∼ 2500 K) are known to display photometric variability in short timescales (hours to days), which has usually been related to rotation-modulated dust cloud patterns, or to unresolved companions. Aims. We perform photometric time-series analysis of a sample of ten early to mid-L dwarfs in the field over three years of Ks-band observations with the OMEGA 2000 infrared camera of the 3.5 m telescope on Calar Alto Observatory between January 2010 and December 2012. This study represents the first systematic long-term photometric monitoring of this kind of object to date. Methods. We perform Ks-band differential photometry of our targets (with typical errors of ±15−30 mmag at the 1σ level) by subtracting a reference flux from each photometric measurement. This reference flux is computed using three nearby, probably constant stars in the target's field-of-view. We then construct and visually inspect the light curves to search for variability, and use four different periodogram algorithms to look for possible periods in our photometric data. Results. Our targets do not display long-term variability over 1σ compared to other nearby stars of similar brightness, nor do the periodograms unveil any possible periodicity for these objects, with two exceptions: 2MASS J02411151-0326587 and G196-3B. In the case of 2MASS J02411151-0326587 (L0), our data suggest a tentative period of 307 ± 21 days, at 40% confidence level, which seems to be associated with peak-to-peak variability of 44 ± 10 mmag. This object may also display variability in timescales of years, as suggested by the comparison of our Ks-band photometry with 2MASS. For G196-3B (L3), we find peak-to-peak variations of 42 ± 10 mmag, with a possible photometric period of 442 ± 7 days, at 95% confidence level. This is roughly the double of the astrometric period reported by Zapatero Osorio et al. (2014, A&A, 568, A6). Given the significance of these results, further photometric data are required to confirm the long-term variability. Conclusions. Our results suggest that early-to mid-L dwarfs are fairly stable in the Ks-band within ±90 mmag at the 3σ level over months to years, which covers hundreds to tens of thousands of rotation cycles. Two out of ten targets show periodic photometric variability at 2.2 µm with peak-to-peak variations of about 40 mmag and tentative periods of ∼300 and ∼450 d.

show abstract

The 2009–2010 fade of Jupiter’s South Equatorial Belt: Vertical cloud structure models and zonal winds from visible imaging

Cited by 39 publications

References 43 publications

Jupiter’s zonal winds and their variability studied with small-size telescopes

Jupiter’s zonal winds and their variability studied with small-size telescopes

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

Long-termKs-band photometric monitoring of L dwarfs

Contact Info

Product

Resources

About