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1 ty of the crust at shallow depths (7 8 km on Europa).
2 exist on other celestial bodies (e.g. Mars, Europa).
3 the genetic variation of bovine S. aureus in Europa.
4 part in the formation of O2 on Ganymede and Europa.
5 nuous oxygen atmosphere has been observed on Europa.
6 me gravity-scaled geometry as those found on Europa.
7 derstanding of the potential habitability of Europa.
8 om other habitable worlds like Enceladus and Europa.
9 erize the habitability of Jupiter's icy moon Europa.
10 ndicating that carbon is sourced from within Europa.
11 core by an internal water ocean like that on Europa.
12 small craters (diameters less than 1 km) on Europa.
13 ust outside the orbit of Jupiter's satellite Europa.
14 n from the jovian footprints of Ganymede and Europa.
15 s are inferred to be folds on Jupiter's moon Europa.
16 l chain would be produced during each day on Europa.
17 ting has played an important role for Io and Europa.
18 distributed on the surface of Jupiter's moon Europa.
19 indirect geological evidence in the case of Europa.
22 y-active worlds, including icy moons such as Europa and Enceladus and exo-planets/moons with high ecc
23 he outer Solar System, such as the icy moons Europa and Enceladus, represent potentially habitable en
25 , discovery of tenuous oxygen atmospheres at Europa and Ganymede and a tenuous carbon dioxide atmosph
26 en the remote observations of the surface of Europa and Ganymede and previously available data on NaC
27 spacecraft observed Jupiter's icy satellites Europa and Ganymede during its flyby in February and Mar
28 of other icy bodies, such as Jupiter's moons Europa and Ganymede, and suggestive of a reservoir of ra
34 idges are the most common surface feature on Europa and occur across every sector of the moon, but th
35 of the primitive Earth, the Jovian satellite Europa and other icy satellites, and the parent body of
36 arse crater population on Jupiter's icy moon Europa and suggest that this assumption is incorrect for
38 ozen water oceans on the moons Enceladus and Europa (and possibly others) and the liquid and frozen h
39 sruption called chaos terrains are unique to Europa, and both their formation and the ice-shell thick
40 from the electromagnetic interactions of Io, Europa, and Ganymede with the magnetospheric plasma flow
43 lcanism on Io, may explain a liquid ocean on Europa, and may guide studies of the dissipative propert
44 The tectonic patterns and stress history of Europa are exceedingly complex and many large-scale feat
46 s previously been detected on the surface of Europa, but it was not possible to determine whether it
47 s an explanation for anomalous radar data on Europa, but until now no penitentes have been identified
48 ations is here modeled as the signature of a Europa-centered dipole moment whose maximum surface magn
50 Urface Dust Analyzer onboard NASA's upcoming Europa Clipper mission at flyby speeds of 4 to 6 kilomet
51 ide the building blocks for life, and NASA's Europa Clipper mission will assess Europa's habitability
53 ration and future data interpretation of the Europa Clipper's SUrface Dust Analyzer (SUDA), which wil
54 Ground-based spectroscopy of Jupiter's moon Europa, combined with gravity data, suggests that the sa
56 internal liquid water oceans in Callisto and Europa, detection of a strong intrinsic magnetic field w
60 o spacecraft's radio carrier wave during two Europa encounters on 19 December 1996 (E4) and 20 Februa
64 simulate multiring basin forming impacts on Europa finding that a total ice shell greater than 20 ki
65 e that although the same orbital position of Europa for plume activity may be a necessary condition,
66 measurements of depths of impact craters on Europa, Ganymede and Callisto that reveal two anomalous
67 ilar situation applies to the galilean moons Europa, Ganymede and Callisto, which reside within Jupit
69 ructure of the four galilean satellites--Io, Europa, Ganymede and Callisto-ranged from uniform mixtur
70 in our understanding of Jupiter's moons Io, Europa, Ganymede, and Callisto over the past few years.
71 s-Europa component shows that, unexpectedly, Europa generates a gas cloud comparable in gas content t
72 we report an analysis of archival data from Europa, guided by processes observed within Earth's subg
73 ently unclear, as is the question of whether Europa has (or had at one time) a liquid water ocean.
74 lts are consistent with the possibility that Europa has a liquid water ocean beneath a surface layer
82 the Galileo spacecraft with the jovian moon Europa have been used to refine models of Europa's inter
83 and that of hydrogen peroxide on neighboring Europa have important implications for understanding wat
84 We infer from these data that Ganymede and Europa have persistent interactions with Jupiter's magne
87 viously unseen emissions arising from Io and Europa in eclipse, a giant volcanic plume over Io's nort
88 subsurface microbial communities on Mars and Europa in which methanogens form the base of the ecosyst
89 54 m per pixel) Galileo spacecraft images of Europa, in which we find evidence for mobile 'icebergs'.
90 ly observed in the optically darker areas of Europa, including the lineaments, and may represent evap
91 erefore, the observation of central peaks on Europa indicates that an ice layer must be sufficiently
93 en topography of Thera Macula indicates that Europa is actively resurfacing over a lens comparable in
96 The ice-rich surface of the jovian satellite Europa is sparsely cratered, suggesting that this moon m
100 ysical mechanisms: the wedge-shaped bands on Europa most probably formed when lower material (ice or
101 The 2014 observations were scheduled with Europa near the apocenter similar to the orbital positio
102 reme radiation (e.g. Mercury, Jupiter's moon Europa, near-Sun comets), as well as terrestrial applica
103 t's magnetometer have indicated that neither Europa nor Callisto have an appreciable internal magneti
104 crometer wavelength region of the surface of Europa obtained by Galileo's Near Infrared Mapping Spect
109 ed at much colder temperatures, meaning that Europa plausibly ended accretion as a mixture containing
112 lstering the case for an exogenous source of Europa's "non-ice" surface material and filling large ga
113 structure of the ice shell and indicate that Europa's at least 20-kilometer ice shell is composed of
114 tions organize in Taylor columns parallel to Europa's axis of rotation, are static inside of the tang
116 from plume activity possibly correlated with Europa's distance from Jupiter through tidal stress vari
120 rue polar wander, involving reorientation of Europa's floating outer ice shell about the tidal axis w
122 ed sulfuric acid concentrations are found in Europa's geologically young terrains, suggesting that lo
123 -synchronous rotation was invoked to explain Europa's global system of lineaments and an equatorial r
126 this model to work, the tensile strength of Europa's ice crust must be less than 40 kilopascals, and
127 the storage and evolution of briny water in Europa's ice shell and propose a framework to interpret
131 ymede and Callisto are equally ice-rich, but Europa's icy shell has a thermal structure about 0.25 0.
133 models to describe the thermal evolution of Europa's interior assuming low initial temperatures (~20
134 t that there may be a permanent asymmetry in Europa's interior mass distribution which is large enoug
135 Occasional eruptions of water sourced from Europa's interior may provide a window on the interior c
136 a from the Galileo mission, many argued that Europa's interior, like Earth, is differentiated into a
139 frared and ultraviolet wavelength spectra of Europa's leading, anti-jovian quadrant observed from the
140 tely 200-km high region well separated above Europa's limb is a firm result and not invalidated by ou
151 his Jovian slot only partially extends along Europa's path, implying that additional, unidentified ac
153 metal core with a radius about 40 percent of Europa's radius surrounded by a rock mantle with a densi
156 c particle bombardment and demonstrates that Europa's surface chemistry is dominated by radiolysis.
157 heir spectral shapes and distribution across Europa's surface indicate that the CO(2) is mixed with o
158 ined by the Voyager spacecraft revealed that Europa's surface is crossed by numerous intersecting rid
159 tures are much higher than those observed on Europa's surface, and an external heating source from th
161 and dark lineaments, suggesting that many of Europa's tectonic patterns may also be related to true p
165 012, the Hubble Space Telescope (HST) imaged Europa's ultraviolet emissions in the search for vapor p
168 board future space missions to Enceladus or Europa, such as the SUrface Dust Analyzer onboard NASA's
169 r-ultraviolet observations of Jupiter's moon Europa taken by Space Telescope Imaging Spectrograph (ST
170 ibe broad arcuate troughs and depressions on Europa that do not fit other proposed stress mechanisms
171 cecraft revealed dark, wedge-shaped bands on Europa that were interpreted as evidence that surface pl
172 interpreted to be similar to those found on Europa, that is, mostly frozen magnesium sulfate brines
174 6 as Galileo passed close to Jupiter's moon, Europa, the magnetometer measured substantial departures
178 ndant NaCl hydrate on icy moon surfaces like Europa, Titan, Ganymede, Callisto, Enceladus, or Ceres.
184 2000, the Galileo spacecraft passed close to Europa when it was located far south of Jupiter's magnet
186 aled the presence of a tenuous ionosphere on Europa, with an average maximum electron density of near
187 thin outer ice shell on Jupiter's large moon Europa would imply easy exchange between the surface and
188 ts with harsher radiation environments, like Europa, would require improved radiation resistance via