&lt;title&gt;The Europa Ocean Discovery mission&lt;/title&gt;

Edwards, B. C.; Chyba, Christopher F.; Abshire, James B.; Burns, Joseph A.; Geissler, P. E.; Konopliv, A. S.; Malin, M. C.; Ostro, S. J.; Rhodes, C. T.; Rudiger, C.; Shao, Xuan-Min; Smith, David E.; Squyres, S. W.; Thomas, P. C.; Uphoff, C.; Walberg, Gerald D.; Werner, Charles; Yoder, C. F.; Zuber, M. T.

doi:10.1117/12.278778

Cited by 4 publications

(4 citation statements)

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“…It has been argued for several years that accurate solutions for the Europan Love numbers k or h could provide definitive evidence of the presence of a liquid ocean beneath the surface ice shell [e.g., Yoder and Sjogren , 1996; Edwards et al , 1997; Chyba et al , 1998; Moore and Schubert , 2000; Wu et al , 2001]. The issue we address in this paper is whether, if there is a liquid ocean, the Love number solutions could be further used to determine the ice thickness, d .…”

Section: Discussionmentioning

confidence: 99%

“…Then, since V T is the sum of spherical harmonics of degree 2 ((1 − 3 cos 2 θ) is a harmonic of degree 2, order 0; sin 2 θ cos (2 λ ) and sin 2 θ sin (2 λ ) are harmonics of degree 2, order 1),

where g is the gravitational acceleration at the European surface and h and k are Love numbers of degree 2 [ Love , 1927; Munk and MacDonald , 1960; Lambeck , 1990]. h and k depend on the internal structure of Europa, and would be much larger if Europa had a liquid ocean than if it did not [see, e.g., Yoder and Sjogren , 1996; Edwards et al , 1997; Chyba et al , 1998; Moore and Schubert , 2000; Wu et al , 2001]. Altimeter observations of tidal surface displacements could provide h , and gravity field solutions for the tidal potential could provide k , and so both measurement types could provide information about the presence of a liquid ocean.…”

Section: Tides and Love Numbersmentioning

confidence: 99%

“…The presence of a liquid ocean would significantly increase tidal amplitudes on Europa [see, e.g., Yoder and Sjogren , 1996; Edwards et al , 1997; Chyba et al , 1998; Moore and Schubert , 2000; Wu et al , 2001]. As a result, measuring tidal amplitudes is one of the primary motivations for a Europa orbiter mission.…”

Section: Introductionmentioning

confidence: 99%

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Tides on Europa, and the thickness of Europa's icy shell

et al. 2006

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[1] It has been shown previously that measurements of tides on Jupiter's moon Europa can be used to determine whether there is a liquid ocean beneath this moon's icy outer shell. In this paper we examine the further possibility of constraining the thickness of the icy shell in the case where a liquid ocean exists, by combining measurements of tidal gravity obtained from tracking an orbiting spacecraft with measurements of vertical tidal surface displacements obtained from a precise onboard altimeter. By simulating a 1-month Europa mapping mission we demonstrate that this combination of tidal measurements would provide a much better estimate of ice thickness than could be obtained using either tracking or altimeter measurements alone. The thickness value inferred from the combined data would also require an estimate of the shear modulus of Europa's icy shell. This introduces an additional uncertainty in the thickness estimate that is approximately proportional to the uncertainty in the inverse of the shear modulus.

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Section: Discussionmentioning

confidence: 99%

Section: Tides and Love Numbersmentioning

confidence: 99%

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Tides on Europa, and the thickness of Europa's icy shell

et al. 2006

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“…And if there is an onboard laser altimeter, it could be used to map out tidal displacements [see, e.g., Smith et al ., ; Neumann et al ., ] and to determine the degree‐2 radial displacement Love number h 2 . Knowledge of either of those Love numbers could provide information on the presence of an ocean beneath the icy outer shell [see, e.g., Yoder and Sjogren , ; Edwards et al ., ; Moore and Schubert , ; Wu et al ., ; Wahr et al ., ], and the two Love numbers could be combined to place constraints on the thickness of the icy shell [ Wahr et al ., ].…”

Section: Introductionmentioning

confidence: 99%

The effects of laterally varying icy shell structure on the tidal response of Ganymede and Europa

Wahr

Zhong

2014

JGR Planets

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We use a finite-element model to solve for the response of Ganymede and Europa to tidal forcing from Jupiter, using various icy shell models with laterally variable (3-D) structure. In all cases, the shell is assumed to be underlain by a liquid-water ocean. Icy shells with laterally varying thickness are derived from a thermal conduction model. Three-dimensional shear modulus profiles for the shell are built either from a conduction model or, for Europa, by assuming a hemispherical difference in composition. Icy shell structures with a nonglobal ocean are built for Ganymede. Using these shell structures to calculate the tidal response of Ganymede and Europa, we conclude the following: (1) the presence of lateral variations in thickness or in shear modulus would not degrade future attempts to use tidal observations to decide on the existence or absence of a liquid ocean and to determine the mean icy shell thickness. (2) Given accurate enough observations, the presence of lateral variations in thickness or in shear modulus could be determined by searching for nondegree-2 components in the tidal response. (3) In the absence of significant viscous convective flow in the shell, the effects of a laterally varying shear modulus on the tidal response would be smaller than those of a laterally varying shell thickness. (4) If the shell is partially grounded, tidal observations of either gravity or uplift would be able to roughly differentiate regions where the ice is grounded from those where it is floating.

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Science Overview of the Europa Clipper Mission

Pappalardo,

Buratti,

Korth

et al. 2024

Space Sci Rev

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The goal of NASA’s Europa Clipper mission is to assess the habitability of Jupiter’s moon Europa. After entering Jupiter orbit in 2030, the flight system will collect science data while flying past Europa 49 times at typical closest approach distances of 25–100 km. The mission’s objectives are to investigate Europa’s interior (ice shell and ocean), composition, and geology; the mission will also search for and characterize any current activity including possible plumes. The science objectives will be accomplished with a payload consisting of remote sensing and in-situ instruments. Remote sensing investigations cover the ultraviolet, visible, near infrared, and thermal infrared wavelength ranges of the electromagnetic spectrum, as well as an ice-penetrating radar. In-situ investigations measure the magnetic field, dust grains, neutral gas, and plasma surrounding Europa. Gravity science will be achieved using the telecommunication system, and a radiation monitoring engineering subsystem will provide complementary science data. The flight system is designed to enable all science instruments to operate and gather data simultaneously. Mission planning and operations are guided by scientific requirements and observation strategies, while appropriate updates to the plan will be made tactically as the instruments and Europa are characterized and discoveries emerge. Following collection and validation, all science data will be archived in NASA’s Planetary Data System. Communication, data sharing, and publication policies promote visibility, collaboration, and mutual interdependence across the full Europa Clipper science team, to best achieve the interdisciplinary science necessary to understand Europa.

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<title>The Europa Ocean Discovery mission</title>

Cited by 4 publications

References 1 publication

Tides on Europa, and the thickness of Europa's icy shell

Tides on Europa, and the thickness of Europa's icy shell

The effects of laterally varying icy shell structure on the tidal response of Ganymede and Europa

Science Overview of the Europa Clipper Mission

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