• Publications
  • Influence
Titan's Rotation Reveals an Internal Ocean and Changing Zonal Winds
Cassini radar observations of Saturn's moon Titan over several years show that its rotational period is changing and is different from its orbital period. The present-day rotation period differenceExpand
  • 166
  • 13
Stochastic Gravitational Wave Background: Upper Limits in the 10–6 to 10–3 Hz Band
We have used precision Doppler tracking of the Cassini spacecraft during its 2001-2002 solar opposition to derive improved observational limits to an isotropic background of low-frequencyExpand
  • 75
  • 6
Jupiter’s interior and deep atmosphere: The initial pole-to-pole passes with the Juno spacecraft
Juno swoops around giant Jupiter Jupiter is the largest and most massive planet in our solar system. NASA's Juno spacecraft arrived at Jupiter on 4 July 2016 and made its first close pass on 27Expand
  • 143
  • 6
  • PDF
The rotation of LAGEOS
In view of the need of an accurate modelling of nongravitational forces on laser-tracked satellites, it is important to understand their rotational dynamics, which determines the temperatureExpand
  • 64
  • 5
  • PDF
A non-hydrostatic Rhea
[1] Radiometric data obtained during Cassini's close flyby of Rhea, on 26 November 2005, has been subject to several published analyses aiming to determine the satellite's mass and quadrupole gravityExpand
  • 24
  • 5
Gravity field and interior of Rhea from Cassini data analysis
Abstract The Cassini spacecraft encountered Rhea on November 26, 2005. Analysis of the Doppler data acquired at and around closest approach yields the mass of Rhea and the quadrupole moments of itsExpand
  • 38
  • 4
Can Cassini detect a subsurface ocean in Titan from gravity measurements
Abstract Recent models of Titan's interior predict that the satellite contains an ocean of water and ammonia under an icy layer. Direct evidence for the presence of an ocean can be provided on theExpand
  • 32
  • 3
The Interior of Saturn
A source of uncertainty in Saturn interior models is the lack of a unique rotation rate to be ascribed to the deep (metallic-hydrogen) interior. As a result, models are not uniquely constrained byExpand
  • 21
  • 3
  • PDF
The Interior of Enceladus
The internal structure of a planetary body provides essential clues about its origin and evolution. Based on its internal density structure, what is the likely composition of the materials from whichExpand
  • 14
  • 2
  • PDF
Current-voltage characteristic of the TSS-1R satellite: Comparison with isotropic and anisotropic models
In this paper we present an analysis of the satellite current-voltage (I-V) characteristics observed during the TSS-IR mission. The satellite I-V curves were compared with the predictions by twoExpand
  • 35
  • 2