Naiara Barrado-Izagirre

• University of the Basque Country

Context . Aerosols are capable of having a huge influence on reflected, emitted, and transmitted planetary spectra, especially at wavelengths similar to their average sizes, but also extending to much longer and shorter wavelengths. The Near InfraRed Spectrograph (NIRSpec) using the PRISM mode on board the James Webb Space Telescope (JWST) is provi...

Aerosols are capable of having a huge influence on reflected, emitted and transmitted planetary spectra. The Near InfraRed Spectrograph (NIRSpec) using the PRISM mode on board of the James Webb Space Telescope (JWST) is providing valuable data of transit spectra over a wide spectral range that is able to cover the whole contribution of aerosols, po...

The transition region between the North Equatorial Band (NEBn) and North Tropical Zone (NTrZ) in Jupiter is home to convective storms, systems of cyclones and anticyclones and atmospheric waves. A large anticyclone formed in the year 2006 at planetographic latitude 19N and persists since then after a complex dynamic history, being possibly the thir...

The transition region between the North Equatorial Band (NEBn) and North Tropical Zone (NTrZ) in Jupiter is home to convective storms, systems of cyclones and anticyclones and atmospheric waves. Zonal winds are weak but have a strong latitudinal shear allowing the formation of cyclones (typically dark) and anticyclones (typically white) that remain...

The banded appearance of Jupiter’s atmosphere shows significant changes over time, sometimes even transforming the reflectivity of a whole latitudinal band in a few weeks, and staying for years with an aspect different from the usual one. The origin of some of these disturbances may be associated with the creation and destruction of the chromophore...

Saturn has an intense and broad eastward equatorial jet with a complex three-dimensional structure mixed with time variability. The equatorial region experiences strong seasonal insolation variations enhanced by ring shadowing, and three of the six known giant planetary-scale storms have developed in it. These factors make Saturn's equator a natura...

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 characteri...

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...

One of the most characteristic feature of Jupiter's atmosphere is its global wind structure which is characterized by strong zonal winds alternating in latitude and correlated with the bright Zones and dark Belts of the planet. This wind system presents a marked temporal stability although the structure of some of its bands change strongly in a qua...

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...

Abstract The general circulation of Jupiter's atmosphere is dominated by a system of zonal winds alternating in latitude and related to the Bands and Zones structure of the planet. The zonal winds have been retrieved in several occasions by analyzing cloud motions in spacecraft observations of the planet and with HST observations [1,3,6,7]. In spit...

The South Equatorial Belt (SEB) of Jupiter is known to alternate its appearance at visible wavelengths from a classical belt-like band most of the time to a short-lived zone-like aspect which is called a “fade” of the belt, hereafter SEBF. The albedo change of the SEB is due to a change in the structure and properties of the clouds and upper hazes....

Jupiter's South Equatorial Belt (SEB) is known to suffer global albedo changes with a not well defined period [1]. The transition from a "belt-like" aspect (low albedo at visible wavelengths) to a "zone-like" (bright albedo) is known as a "Fade". During 2009 the SEB suffered a fading process and became completely transformed to a zone by the first...

We present a study of the long-term evolution of the cloud of aerosols produced in the atmosphere of Jupiter by the impact of an object on 19 July 2009 (Sánchez-Lavega, A. et al. [2010]. Astrophys. J. 715, L155–L159). The work is based on images obtained during 5months from the impact to 31 December 2009 taken in visible continuum wavelengths and f...

We present a study of the equatorial region of Jupiter, between latitudes ∼15°S and ∼15°N, based on Cassini ISS images obtained during the Jupiter flyby at the end of 2000, and HST images acquired in May and July 2008. We examine the structure of the zonal wind profile and report the detection of significant longitudinal variations in the intensity...

We have studied the equatorial region of Jupiter, between 15ºS and 15ºN, on Cassini ISS images obtained during the Jupiter flyby at the end of 2000 and on HST images acquired in May and July 2008. We have found significant longitudinal variations in the intensity of the 6ºN eastward jet, up to 60 m s-1 in Cassini and HST observations. In the HST ca...

We have studied the spatial distribution of Jupiter’s higher clouds in order to characterize the turbulent regime and the presence of waves in this planet’s atmosphere. We have used images from the Hubble Space Telescope (HST) 1995’s archive and from Cassini’s ISS camera during its Jupiter fly-by in its way to Saturn in 2000 in three wavelengths: n...

Aims. Despite the banded visual aspect of cloud patterns in Jupiter, high resolution images indicate that these regions are markedly turbulent. One region of particular interest is the north temperate belt (NTB) at 21◦ N planetocentric latitude, where the most intense Jovian jet resides with eastward peak speeds of 160 - 180 ms−1. Almost every 15 y...

The banded visual aspect of cloud patterns in Jupiter hides markedly turbulent areas visible in high resolution images. The North Temperate Belt (NTB) at 21° N planetocentric latitude where the most intense Jovian jet resides (with speeds of 160 - 180 m/s) is a region of particular interest because it is known to suffer almost every 15 years an eru...

In this work we analyze the spatial structure of Jupiter's cloud reflectivity field in order to determine brightness periodicities and power spectra characteristics together with their relationship with Jupiter's dynamics and turbulence. The research is based on images obtained in the near-infrared (∼950 nm), blue (∼430 nm) and near-ultraviolet (∼2...

The analysis of the brightness spectral distribution of the fully cloud covered atmosphere of Jupiter provides an essential information on the characteristic spatial scales of atmospheric features and their distribution. As previously proposed by other authors, the analysis of the brightness power spectra can be used as an approximation to the kine...

The main goal of this work is to study the brightness field in Jupiter in order to characterize its periodicities and power spectral distribution, and relate them with the dynamics and turbulence of the atmosphere. To do so we have used two sets of images obtained in the near-infrared (~950 nm, NIR), blue (430 nm, BL) and ultraviolet (~260, UV). Th...

For a variety of reasons, Jupiter's polar areas are probably the less observed regions of the planet. To study the dynamics and cloud vertical structure in the polar regions of the planet (latitudes 50° to 80° in both hemispheres) we have used images of Jupiter obtained from the ultraviolet to near infrared (258 to 939 nm) by the Cassini Imagining...

The morphology of cloud forms in Jupiter's atmosphere is rich in a variety of temporal and spatial scales. Analysis of their brightness distribution can be used as diagnose of the turbulence spectrum in Jupiter's atmosphere. We have used Hubble Space Telescope images at wavelength of 953 nm continuum filter sensitive to the upper ammonia cloud obta...

We have used high resolution images of Jupiter obtained by Cassini-ISS instrument in the CB2 filter during its flyby of the planet in December 2000, to measure the motions of cloud features between latitudes ±50º to ±80º. Maps of the poles have been constructed to identify and track cloud features in successive image frames. Two techniques have bee...

Jupiter's South Equatorial Belt (SEB) is known to suffer global albedo changes with a not well defined period [1]. The transition from a "belt-like" aspect (low albedo at visible wavelengths) to a "zone-like" (bright albedo) is known as a "Fade". During 2009 the SEB suffered a fading process and became completely transformed to a zone by the first...