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|a Weiss, Benjamin P.
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|a Biersteker, John B.
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|a Colicci, Vittorio
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|a Goode, Allison
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|a Castillo‐Rogez, Julie C.
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|a Petropoulos, Anastassios E.
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|a Balint, Tibor S.
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|a Searching for Subsurface Oceans on the Moons of Uranus Using Magnetic Induction
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|b American Geophysical Union (AGU),
|c 2022-02-16T19:01:46Z.
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|z Get fulltext
|u https://hdl.handle.net/1721.1/140437
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|a The icy moons of Uranus may contain subsurface oceans. Such oceans could be detected and characterized using measurements of magnetic fields induced by Uranus' time-varying magnetospheric field. Here we explore this possibility for Uranus's five major moons, with a focus on Ariel. We find that the magnetic field at each moon is dominated by the synodic frequency with amplitudes ranging from ∼4 nT at Oberon up to ∼300 nT at Miranda. If these bodies contain oceans with sufficient thicknesses (>∼3-40 km) and conductivities (>2 S m−1) even underlying relatively thick (∼50 km) ice shells, the induced surface fields should have amplitudes exceeding the typical ∼1 nT sensitivity of spacecraft magnetometry investigations. Furthermore, the magnetic field variations at the moons span periods ranging from 1 to 103 h. These could enable long-term measurements to separately constrain ocean and ice thicknesses and ocean salinity.
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|a Article
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|t Geophysical Research Letters
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