ライフサイエンスコーパス: Europa

1 exist on other celestial bodies (e.g. Mars, Europa).

2 ty of the crust at shallow depths (7 8 km on Europa).

3 core by an internal water ocean like that on Europa.

4 small craters (diameters less than 1 km) on Europa.

5 ust outside the orbit of Jupiter's satellite Europa.

6 n from the jovian footprints of Ganymede and Europa.

7 s are inferred to be folds on Jupiter's moon Europa.

8 l chain would be produced during each day on Europa.

9 ting has played an important role for Io and Europa.

10 distributed on the surface of Jupiter's moon Europa.

11 indirect geological evidence in the case of Europa.

12 part in the formation of O2 on Ganymede and Europa.

13 nuous oxygen atmosphere has been observed on Europa.

14 inner magnetosphere) in the vicinity of both Europa and Callisto.

15 , discovery of tenuous oxygen atmospheres at Europa and Ganymede and a tenuous carbon dioxide atmosph

16 spacecraft observed Jupiter's icy satellites Europa and Ganymede during its flyby in February and Mar

17 of other icy bodies, such as Jupiter's moons Europa and Ganymede, and suggestive of a reservoir of ra

18 tenuous oxygen atmospheres recently found on Europa and Ganymede.

19 aturn like that which links Jupiter with Io, Europa and Ganymede.

20 ayer of O2 gas similar to the atmospheres of Europa and Ganymede.

21 aplace resonance linking Jupiter's moons Io, Europa and Ganymede.

22 of the primitive Earth, the Jovian satellite Europa and other icy satellites, and the parent body of

23 arse crater population on Jupiter's icy moon Europa and suggest that this assumption is incorrect for

24 ds may compensate for extension elsewhere on Europa and then relax away over time.

25 ozen water oceans on the moons Enceladus and Europa (and possibly others) and the liquid and frozen h

26 sruption called chaos terrains are unique to Europa, and both their formation and the ice-shell thick

27 e the mean orbital angular velocities of Io, Europa, and Ganymede, respectively.

28 lcanism on Io, may explain a liquid ocean on Europa, and may guide studies of the dissipative propert

29 The tectonic patterns and stress history of Europa are exceedingly complex and many large-scale feat

30 The appearances of the craters on Europa are inconsistent with thin-ice-shell models and i

31 s an explanation for anomalous radar data on Europa, but until now no penitentes have been identified

32 ations is here modeled as the signature of a Europa-centered dipole moment whose maximum surface magn

33 Ground-based spectroscopy of Jupiter's moon Europa, combined with gravity data, suggests that the sa

34 The trans-Europa component shows that, unexpectedly, Europa genera

35 internal liquid water oceans in Callisto and Europa, detection of a strong intrinsic magnetic field w

36 observations of Jupiter's Galilean satellite Europa during its tour of the jovian system.

37 o spacecraft's radio carrier wave during two Europa encounters on 19 December 1996 (E4) and 20 Februa

38 everal impact craters on Jupiter's satellite Europa exhibit central peaks.

39 Visual wavelength images of Europa extend knowledge of its global pattern of arcuate

40 e that although the same orbital position of Europa for plume activity may be a necessary condition,

41 measurements of depths of impact craters on Europa, Ganymede and Callisto that reveal two anomalous

42 ilar situation applies to the galilean moons Europa, Ganymede and Callisto, which reside within Jupit

43 ters one of the four galilean satellites-Io, Europa, Ganymede and Callisto-on each orbit.

44 ructure of the four galilean satellites--Io, Europa, Ganymede and Callisto-ranged from uniform mixtur

45 in our understanding of Jupiter's moons Io, Europa, Ganymede, and Callisto over the past few years.

46 s-Europa component shows that, unexpectedly, Europa generates a gas cloud comparable in gas content t

47 we report an analysis of archival data from Europa, guided by processes observed within Earth's subg

48 ently unclear, as is the question of whether Europa has (or had at one time) a liquid water ocean.

49 lts are consistent with the possibility that Europa has a liquid water ocean beneath a surface layer

50 The metallic core is favored if Europa has a magnetic field.

51 The quantity of gas found indicates that Europa has a much greater impact than hitherto believed

52 The measurements indicate that Europa has a predominantly water ice-liquid outer shell

53 However, Europa has a small forced eccentricity e approximately 0

54 the Galileo spacecraft with the jovian moon Europa have been used to refine models of Europa's inter

55 We infer from these data that Ganymede and Europa have persistent interactions with Jupiter's magne

56 ns of the outer planets, with Jupiter's moon Europa having received the most attention.

57 viously unseen emissions arising from Io and Europa in eclipse, a giant volcanic plume over Io's nort

58 subsurface microbial communities on Mars and Europa in which methanogens form the base of the ecosyst

59 54 m per pixel) Galileo spacecraft images of Europa, in which we find evidence for mobile 'icebergs'.

60 ly observed in the optically darker areas of Europa, including the lineaments, and may represent evap

61 erefore, the observation of central peaks on Europa indicates that an ice layer must be sufficiently

62 en topography of Thera Macula indicates that Europa is actively resurfacing over a lens comparable in

63 Europa is most likely differentiated into a metallic cor

64 The ice-rich surface of the jovian satellite Europa is sparsely cratered, suggesting that this moon m

65 ysical mechanisms: the wedge-shaped bands on Europa most probably formed when lower material (ice or

66 The 2014 observations were scheduled with Europa near the apocenter similar to the orbital positio

67 t's magnetometer have indicated that neither Europa nor Callisto have an appreciable internal magneti

68 crometer wavelength region of the surface of Europa obtained by Galileo's Near Infrared Mapping Spect

69 pots-discovered in high-resolution images of Europa obtained by the Galileo spacecraft.

70 a obtained on 8 March 2015 ut as the limb of Europa occulted Io.

71 Close to Europa, plasma currents appear to produce perturbations

72 h scale sizes that are small compared with a Europa radius.

73 lstering the case for an exogenous source of Europa's "non-ice" surface material and filling large ga

74 from plume activity possibly correlated with Europa's distance from Jupiter through tidal stress vari

75 d 20 February 1997 (E6) were used to measure Europa's external gravitational field.

76 The evidence that Europa's field varies temporally strengthens the argumen

77 rue polar wander, involving reorientation of Europa's floating outer ice shell about the tidal axis w

78 ed sulfuric acid concentrations are found in Europa's geologically young terrains, suggesting that lo

79 -synchronous rotation was invoked to explain Europa's global system of lineaments and an equatorial r

80 Spectra of Europa's high latitudes imply that fine-grained water fr

81 this model to work, the tensile strength of Europa's ice crust must be less than 40 kilopascals, and

82 ng liquid water to estimate the thickness of Europa's icy crust.

83 ymede and Callisto are equally ice-rich, but Europa's icy shell has a thermal structure about 0.25 0.

84 ns on all three satellites, which constrains Europa's icy shell to be at least 19 km thick.

85 t that there may be a permanent asymmetry in Europa's interior mass distribution which is large enoug

86 on Europa have been used to refine models of Europa's interior.

87 a permanent magnetic dipole moment model of Europa's internal field.

88 frared and ultraviolet wavelength spectra of Europa's leading, anti-jovian quadrant observed from the

89 tely 200-km high region well separated above Europa's limb is a firm result and not invalidated by ou

90 If Europa's orbit were circular, or the satellite were comp

91 depend on changing surface stresses based on Europa's orbital phases.

92 nse to diurnal variations in tidal stress in Europa's outer ice shell.

93 The thickness of Europa's outer shell of water ice-liquid must lie in the

94 e mantle by a liquid magma ocean, similar to Europa's present ice shell.

95 metal core with a radius about 40 percent of Europa's radius surrounded by a rock mantle with a densi

96 it could be as large as about 50 percent of Europa's radius.

97 The dipole orientation is oblique to Europa's spin axis.

98 c particle bombardment and demonstrates that Europa's surface chemistry is dominated by radiolysis.

99 ined by the Voyager spacecraft revealed that Europa's surface is crossed by numerous intersecting rid

100 tures are much higher than those observed on Europa's surface, and an external heating source from th

101 acid is present and is a major component of Europa's surface.

102 and dark lineaments, suggesting that many of Europa's tectonic patterns may also be related to true p

103 Galileo observations of Europa's thermal emission show low-latitude diurnal brig

104 mation and the ice-shell thickness depend on Europa's thermal state.

105 It has been suggested that Europa's thin outer ice shell might be separated from th

106 012, the Hubble Space Telescope (HST) imaged Europa's ultraviolet emissions in the search for vapor p

107 these minerals provide a close match to the Europa spectra.

108 We find evidence that Europa spins faster than the synchronous rate (or did so

109 r-ultraviolet observations of Jupiter's moon Europa taken by Space Telescope Imaging Spectrograph (ST

110 ibe broad arcuate troughs and depressions on Europa that do not fit other proposed stress mechanisms

111 cecraft revealed dark, wedge-shaped bands on Europa that were interpreted as evidence that surface pl

112 interpreted to be similar to those found on Europa, that is, mostly frozen magnesium sulfate brines

113 Europa, the innermost icy satellite of Jupiter, has a to

114 6 as Galileo passed close to Jupiter's moon, Europa, the magnetometer measured substantial departures

115 In the specific case of Europa, the minimum kinetic energy of the flow associate

116 led as contributions of an internal field of Europa, they do not confirm its existence.

117 Currents coupling Europa to Jupiter's magnetospheric plasma could produce

118 The plume was present when Europa was near apocenter and was not detected close to

119 Non-synchronous rotation of Europa was predicted on theoretical grounds, by consider

120 2000, the Galileo spacecraft passed close to Europa when it was located far south of Jupiter's magnet

121 aled the presence of a tenuous ionosphere on Europa, with an average maximum electron density of near

122 thin outer ice shell on Jupiter's large moon Europa would imply easy exchange between the surface and