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Pierre-Louis Phan

Publications and source records attributed to Pierre-Louis Phan.

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Kilometre-scale Jovian moon characterized for a potential JUICE flyby

Jupiter's irregular satellites are thought to be relics of early Solar System planetesimals. However, their small sizes, large distances from Earth and close angular proximity to Jupiter make them difficult to characterize remotely. Here we report multi-instrument observations of kilometre-sized Kallichore, the only irregular moon of Jupiter amenable to a close flyby by ESA's Jupiter Icy Moons Explorer (JUICE), whose astrometric and physical properties were still poorly constrained. We used Hubble photometry and astrometry, followed by a ground-based, multi-site stellar occultation campaign and astrometric and photometric observations with the 10.4-m Gran Telescopio Canarias. We reduced Kallichore's orbital uncertainty by up to approximately 80% and determined its shape: an elongated object with a minimum semi-axis ratio of a/b = 1.53 +/- 0.10, an area-equivalent diameter of 3.8 (+2.3/-0.3) km and a dark surface with a geometric albedo of 3.7% (+0.7/-2.2). No close companions were detected. These new constraints provide a viable pathway towards a JUICE flyby once the spacecraft arrives in the Jupiter system in 2031.

astro-ph.EP

Polar motion of Venus

Five Venus missions are under development to study the planet in the next decade, with both NASA's VERITAS and ESA's EnVision featuring a geophysical investigation among their objectives. Their radar and gravity experiments will determine Venus's orientation, enabling analyses of its spin dynamics to infer relevant geophysical and atmospheric properties. This work aims to characterize Venus's polar motion, defined as the motion of its spin axis in a body-fixed frame. We focus on signatures from its interior and atmosphere to support potential detections of polar motion by future orbiters. We developed a polar motion model for a triaxial planet accounting for solar torque, centrifugal and tidal deformations of a viscoelastic mantle, and atmospheric dynamics. Core-mantle coupling effects were analyzed separately, considering a simplified spherical core. We computed the period and damping time of the free motion (i.e., the Chandler wobble) and determined the frequencies and amplitudes of the forced motion. We revisited the Chandler frequency expression. Solar torque is the dominant phenomenon affecting Venus's Chandler frequency, increasing it by a factor of 2.75. Our model predicts a Chandler period in the range [12900 ; 18900] years. The Chandler wobble appears as a linear polar drift of about 90 meters on Venus's surface during EnVision's 4-year primary mission, at the limit of its resolution. We also predict forced polar motion oscillations with an amplitude of about 20 meters, driven by the atmosphere and the solar torque. Compared to the 240 meter spin axis precession occurring in inertial space over this duration, these results suggest that Venus's polar motion could also be detectable by future orbiters. Polar motion should be incorporated into rotation models when anticipating these missions, providing additional constraints on the interior structure of Venus.

astro-ph.EP