Results 11 to 20 of about 33,171 (317)

Tilting Uranus via the migration of an ancient satellite [PDF]

A&A 668, A108 (2022), 2022
Context. The 98{\deg}-obliquity of Uranus is commonly attributed to giant impacts that occurred at the end of the planetary formation. This picture, however, is not devoid of weaknesses. Aims. On a billion-year timescale, the tidal migration of the satellites of Jupiter and Saturn has been shown to strongly affect their spin-axis dynamics.
M. Saillenfest, Zeeve Rogoszinski, G. Lari, Kevin Bailli'e, G. Bou'e, A. Crida, V. Lainey   +6 more
arxiv   +3 more sources

The Case for a New Frontiers–Class Uranus Orbiter: System Science at an Underexplored and Unique World with a Mid-scale Mission

The Planetary Science Journal, 2022
Current knowledge of the Uranian system is limited to observations from the flyby of Voyager 2 and limited remote observations. However, Uranus remains a highly compelling scientific target due to the unique properties of many aspects of the planet ...
Ian J. Cohen, Chloe Beddingfield, Robert Chancia, Gina DiBraccio, Matthew Hedman, Shannon MacKenzie, Barry Mauk, Kunio M. Sayanagi, Krista M. Soderlund, Elizabeth Turtle, Caitlin Ahrens, Christopher S. Arridge, Shawn M. Brooks, Emma Bunce, Sebastien Charnoz, Athena Coustenis, Robert A. Dillman, Soumyo Dutta, Leigh N. Fletcher, Rebecca Harbison, Ravit Helled, Richard Holme, Lauren Jozwiak, Yasumasa Kasaba, Peter Kollmann, Statia Luszcz-Cook, Kathleen Mandt, Olivier Mousis, Alessandro Mura, Go Murakami, Marzia Parisi, Abigail Rymer, Sabine Stanley, Katrin Stephan, Ronald J. Vervack, Jr., Michael H. Wong, Peter Wurz   +36 more
doaj   +2 more sources

Empirical Structure Models of Uranus and Neptune [PDF]

Monthly notices of the Royal Astronomical Society, 2022
Uranus and Neptune are still poorly understood. Their gravitational fields, rotation periods, atmosphere dynamics, and internal structures are not well determined. In this paper we present empirical structure models of Uranus and Neptune where the density profiles are represented by polytropes.
Benno A. Neuenschwander, R. Helled
arxiv   +3 more sources

Linking Uranus' temperature profile to wind-induced magnetic fields [PDF]

Monthly notices of the Royal Astronomical Society, 2021
The low luminosity of Uranus is still a puzzling phenomenon and has key implications for the thermal and compositional gradients within the planet. Recent studies have shown that planetary volatiles become ionically conducting under conditions that are present in the ice giants. Rapidly growing electrical conductivity with increasing depth would couple
Deniz Soyuer, R. Helled
arxiv   +3 more sources

Explaining the low luminosity of Uranus: A self-consistent thermal and structural evolution [PDF]

A&A 633, A50 (2020), 2019
The low luminosity of Uranus is a long-standing challenge in planetary science. Simple adiabatic models are inconsistent with the measured luminosity, which indicates that Uranus is non-adiabatic because it has thermal boundary layers and/or conductive regions.
A. Vazan, R. Helled
arxiv   +3 more sources

Combination of Density‐Based Spatial Clustering With Grid Search Using Nash Equilibrium

Engineering Reports
This paper introduces a novel clustering approach that enhances the traditional Density‐Based Spatial Clustering of Applications with Noise (DBSCAN) algorithm by integrating a grid search method and Nash Equilibrium principles and addresses the ...
Uranus Kazemi, Seyfollah Soleimani
doaj   +2 more sources

Constraining the effect of convective inhibition on the thermal evolution of Uranus and Neptune [PDF]

arXiv, 2021
The internal heat flows of both Uranus and Neptune remain major outstanding problems in planetary science. Uranus' surprisingly cold effective temperature is inconsistent with adiabatic thermal evolution models, while Neptune's substantial internal heat flow is twice its received insolation.
S. Markham, D. Stevenson
arxiv   +3 more sources

The Satellites of Uranus [PDF]

International Astronomical Union Colloquium, 1982
AbstractThe Uranian satellite system contains five known members, all of which are difficult to study owing to their faintness and proximity to Uranus. The photometry of these objects is not in a satisfactory state, nor is the photovisual spectrophotometry.
D. P. Cruikshank
openalex   +3 more sources

The Magnetosphere of Uranus [PDF]

International Astronomical Union Colloquium, 1982
The magnetosphere of a planet, as the name implies, is the region surrounding the planet in which the planetary magnetic field plays a dominant role in determining the behaviour of the medium. The inner boundary of a magnetosphere is the surface of the planet if it has no significant atmosphere (as in the case of Mercury), or the lower ionosphere in ...
W. I. Axford
openalex   +3 more sources

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 disk, Neptune's moons are irregular and are captured objects.
Christian Reinhardt, A. Chau, J. Stadel, R. Helled   +3 more
arxiv   +3 more sources