Results 91 to 100 of about 11,862 (238)
Proceedings of the National Academy of Sciences of the United States of America, 2020 Significance Understanding the interior structure and dynamics of outer Solar System planets in terms of their component materials is a major scientific challenge.
Peihao Huang +8 more
semanticscholar +1 more source
On the Detection of Low‐Frequency Planetary Radio Emission With an Orbiting Interferometer
Radio Science, Volume 61, Issue 6, June 2026.Abstract The magnetized planets of the outer Solar System produce kilometric radio emissions at very low frequencies (<1 ${< } 1\,$MHz). They reveal the planetary magnetic dynamics and their interaction with the solar wind. Those radio emissions can also serve as a proxy for interplanetary space weather monitoring.
E. Rouillé +4 more
wiley +1 more source
Strong Tidal Dissipation at Uranus?
The Planetary Science Journal, 2023 Geophysical estimates of paleo heat fluxes on the Uranian moons Miranda and Ariel are in the range of 25–75 mW m ^−2 . For a canonical Uranus dissipation factor Q = 18,000, expected equilibrium tidal heating rates for these satellites are less than 6 mW ...
Francis Nimmo
doaj +1 more source
Rotation‐Controlled Diurnal Evolution of Uranus' Asymmetric Bow Shock at Equinox
AGU Advances, Volume 7, Issue 3, June 2026.Abstract Uranus possesses the most extreme magnetic and rotational geometry in the solar system, resulting in a uniquely dynamic and asymmetric interaction between its magnetosphere and the solar wind. Here we investigate the diurnal evolution of the Uranian bow shock (BS) at equinox using global multifluid magnetohydrodynamic simulations constrained ...
X. Cao, C. Paty, F. Chu, J. Lei
wiley +1 more source
katelinbdonaldson/KHIs-at-Uranus-and-Neptune: KHIs at Uranus and Neptune
<p>This repository includes the scripts used to create analytic model to produce the results in the paper "Characterizing the solar wind-magnetosphere viscous interaction at Uranus and Neptune".</p> <p>The MATLAB code is split
katelinbdonaldson
core +1 more source
Ultraviolet geometric albedo of Uranus [PDF]
, 1988 The purpose was to obtain ultraviolet flux measurements of Uranus before and after the January 1986 flyby past Uranus by Voyager. These measurements were used to determine absolute flux distributions in the wavelength range 1950 to 3200 A.
Neff, John S.
core
Different Inhomogeneous Evolutionary Histories for Uranus and Neptune
The Astrophysical Journal LettersWe present updated nonadiabatic and inhomogeneous evolution models for Uranus and Neptune, employing an interior composition of methane, ammonia, water, and rocks.
Roberto Tejada Arevalo
doaj +1 more source
Journal of Geophysical Research: Space Physics, Volume 131, Issue 6, June 2026.Abstract We present large‐scale simulations of energetic neutral atom (ENA) emissions at Uranus from a spacecraft viewpoint. Models of magnetic field, extended hydrogen exosphere, moon‐sourced neutral tori, and proton radiation belt are implemented into a simulator to evaluate the production of ENAs for L $L$ = 1–15.
D. Santos‐Costa, N. André
wiley +1 more source
Uranus, Neptune, and Exoplanets
, 2013 This chapter focuses on the climates of Uranus, Neptune, and exoplanets. Uranus spins on its side, which allows a comparison between sunlight and rotation for their effects on weather patterns. In contrast to Venus, Uranus is only weakly affcted by tides
Andrew P. Ingersoll
core +1 more source
Bifurcation in the history of Uranus and Neptune: the role of giant impacts [PDF]
Monthly notices of the Royal Astronomical Society, 2019 Despite many similarities, there are significant observed differences between Uranus and Neptune: While Uranus is tilted and has a regular set of satellites, suggesting their accretion from a disc, Neptune’s moons are irregular and are captured objects.
Christian Reinhardt +3 more
semanticscholar +1 more source