scholarly journals Robotic Autonomous Spacecraft Missions: Cassini Mission-To-Saturn Example

2019 ◽  
Author(s):  
Paula S. Morgan
Keyword(s):  
Cassini Mission

Qualifying and testing HASI-STUB for Huygens-Cassini Mission

1996 ◽  
Author(s):  
F. Angrilli ◽  
G. Bianchini ◽  
S. Debei ◽  
G. Fanti ◽  
B. Saggin
Keyword(s):  
Cassini Mission

The CRAF/Cassini mission: Baseline plan and status

1992 ◽  
Author(s):  
Reed E. Wilcox ◽  
Dougals S. Abraham ◽  
C. Perry Bankston ◽  
Sandra M. Dawson ◽  
John W. Klein ◽  
...  
Keyword(s):  
Cassini Mission

scholarly journals Comparison of the deep atmospheric dynamics of Jupiter and Saturn in light of the Juno and Cassini gravity measurements

2020 ◽  
Author(s):  
Yohai Kaspi ◽  
Eli Galanti ◽  
Adam Showman ◽  
David Stevenson ◽  
Tristan Guillot ◽  
...  
Keyword(s):  
Planetary Science ◽  
Gravity Inversion ◽  
Zonal Flows ◽  
Zonal Jets ◽  
Cassini Mission ◽  
Gravity Measurements ◽  
Order Of Magnitude ◽  
The Magnetic Field ◽  
Intrinsic Characteristic

<p>The nature and structure of the observed east-west flows on Jupiter and Saturn has been a long-standing mystery in planetary science. This mystery has been recently unraveled by the accurate gravity measurements provided by the Juno mission to Jupiter and the Grand Finale of the Cassini mission to Saturn. These two experiments, which coincidentally happened around the same time, allowed the determination of the overall vertical and meridional profiles of the zonal flows on both planets. In this talk, we discuss what has been learned about the zonal jets on the gas giants in light of the new data from these two experiments. The gravity measurements not only allow the depth of the jets to be constrained, yielding the inference that the jets extend to roughly 3000 and 9000 km below the observed clouds on Jupiter and Saturn, respectively, but also provide insights into the mechanisms controlling these zonal flows. Specifically, for both planets this depth corresponds to the depth where electrical conductivity is within an order of magnitude of 1 S/m, implying that the magnetic field likely plays a key role in damping the zonal flows. An intrinsic characteristic of any gravity inversion, as discussed here, is that the solutions might not be unique. We analyze the robustness of the solutions and present several independent lines of evidence supporting the inference that the jets reach these depths.</p>

Boom structure optimization for HASI on Cassini mission

1994 ◽  
Author(s):  
F. Reccanello ◽  
G. Fanti ◽  
F. Angrilli
Keyword(s):  
Structure Optimization ◽  
Cassini Mission

Evolution of Titan’s stratosphere with Cassini/CIRS

2021 ◽  
Author(s):  
Athena Coustenis ◽  
Donald Jennings ◽  
Richard Achterberg ◽  
Panayotis Lavvas ◽  
Conor Nixon ◽  
...  
Keyword(s):  
High Resolution ◽  
Chemical Species ◽  
Far Infrared ◽  
Organic Content ◽  
Large Temperature ◽  
Neutral Atmosphere ◽  
South Pole ◽  
The South ◽  
The North ◽  
Cassini Mission

<p>Titan is a unique body in the solar system in particular because of its earth-like surface features, its putative undersurface liquid water ocean and its large organic content in the atmosphere and on the surface . These chemical species evolve with season, as Titan follows Saturn in its orbit around the Sun with an inclination of about 27°. We performed an analysis of spectra acquired by Cassini/CIRS at high resolution covering the range from 10 to 1500 cm<sup>-1</sup> since the beginning and until the last flyby of Titan in 2017 and describe the temperature and composition variations ([1-3]. By applying our radiative transfer code (ARTT) to the high-resolution CIRS spectra we study the stratospheric evolution over almost two Titan seasons [1,2]. CIRS nadir and limb spectral together show variations in temperature and chemical composition in the stratosphere during the Cassini mission, before and after the Northern Spring Equinox (NSE) and also during one Titan year.</p><p>Since the 2010 equinox we have thus reported on monitoring of Titan’s stratosphere near the poles and in particular on the observed strong temperature decrease and compositional enhancement above Titan’s southern polar latitudes since 2012 and until 2014 of several trace species, such as complex hydrocarbons and nitriles, which were previously observed only at high northern latitudes. This effect followed the transition of Titan’s seasons from northern winter in 2002 to northern summer in 2017, while at that latter time the southern hemisphere was entering winter.</p><p>Our data show a continued decrease of the abundances which we first reported to have started in 2015. The 2017 data we have acquired and analyzed here are important because they are the only ones recorded since 2014 close to the south pole in the far-infrared nadir mode at high resolution. A large temperature increase in the southern polar stratosphere (by 10-50 K in the 0.5 mbar-0.05 mbar pressure range) is found and a change in the temperature profile’s shape. The 2017 observations also show a related significant decrease in most of the abundances which must have started sometime between 2014 and 2017 [3]. In our work, we show that the equatorial latitudes remain rather constant throughout the Cassini mission.</p><p>We have thus shown that the south pole of Titan is now losing its strong enhancement, while the north pole also slowly continues its decrease in gaseous opacities. It would have been interesting to see when this might happen, but the Cassini mission ended in September 2017. Perhaps future ground-based measurements and the Dragonfly mission can pursue this investigation and monitor Titan’s atmosphere to characterize the seasonal events. Our results set constraints on GCM and photochemical models.</p><p>References:</p><p> [1] Coustenis et al., 2016, Icarus 270, 409-420; [2] Coustenis et al., 2018, Astroph. J., Lett., 854, no2; [3] Coustenis et al., 2020. Titan’s neutral atmosphere seasonal variations up to the end of the Cassini mission. Icarus 344, 113413. https://doi.org/10.1016/j.icarus.2019.113413.</p>

NASA extends Cassini mission

Physics World ◽  
2008 ◽  
Vol 21 (05) ◽  
pp. 10-10
Keyword(s):  
Cassini Mission

How does the Sun Influence the Magnetospheres of Jupiter and Saturn?

2017 ◽  
Vol 13 (S335) ◽  
pp. 109-113
Author(s):  
Caitríona M. Jackman ◽  
Christopher S. Arridge
Keyword(s):  
Solar Wind ◽  
Solar Cycle ◽  
Dynamic Pressure ◽  
Current Data ◽  
Data Streaming ◽  
Cassini Mission ◽  
Flux Variability ◽  
Solar Uv ◽  
Complete Set ◽  
The Impact

AbstractSpacecraft have visited Jupiter and Saturn at all phases of the solar cycle and thus we have a wealth of data with which to explore both upstream parameters and magnetospheric response. In this paper we review upstream parameters including interplanetary magnetic field strength and direction, solar wind dynamic pressure, plasma beta and Mach number. We consider the impact of changing solar wind on dayside coupling via reconnection. We also comment on how solar UV flux variability over a solar cycle influences the plasma and neutral tori in the inner magnetospheres of Jupiter and Saturn, and thus estimate the solar cycle effects on internally driven magnetospheric dynamics. Finally we place our results in the context of the now complete set of data from the Cassini mission at Saturn and the current data streaming in from Juno at Jupiter, outlining future avenues for research.

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