ライフサイエンスコーパス: Io

1 Io experiences tidal deformation as a result of its ecce

2 Io joins a growing list of bodies with tenuous and trans

3 Io leaves a magnetic footprint on Jupiter's upper atmosp

4 Io's disk-averaged emission diminishes with time after e

5 ffuse emission extending to approximately 20 Io radii.

6 tate 13-acetate (PMA) plus ionophore A23187 (Io), which induces NFAT activation, increased REDD1 mRNA

7 ers per pixel) images of volcanically active Io.

8 We found that all 'Io occupied a relatively small geographic area, their pl

9 d known solid planetary body-after Earth and Io-that is sufficiently geologically active for its inte

10 low subsurface interactions between lava and Io's widespread sulfur dioxide (SO(2)) frost can produce

11 o measure and is only known for the Moon and Io.

12 f amplitude consistent with dynamo action at Io would explain the observations.

13 The plasma conditions at Io appear to account for the decrease in the magnetic fi

14 agnetic field to form a co-rotating torus at Io's distance; the remaining ions and electrons form Io'

15 outburst shows that the interaction between Io and Jupiter's magnetosphere is stabilized by a feedba

16 parent plasmoids-and contains ions from both Io and Jupiter's ionosphere with intense bursts of H(+)

17 ong the trajectory as the spacecraft flew by Io.

18 The Galileo orbiter's close pass by Io in 1995 produced evidence for extensive mass loading

19 solar component is absorbed more strongly by Io because its gyroradius is smaller than Io's diameter.

20 otprint of the magnetic flux tube connecting Io to Jupiter.

21 sland of Hawai'i, Hawai'i, USA, the endemic 'Io, or Hawaiian Hawk (Buteo solitarius), is a species of

22 bstrate was evident by both the extrapolated Io scattering and radius of gyration and was supported b

23 dal heating has played an important role for Io and Europa.

24 , which provides a primary energy source for Io's continuing volcanic activity and infrared emission(

25 tance; the remaining ions and electrons form Io's ionosphere.

26 ibe previously unseen emissions arising from Io and Europa in eclipse, a giant volcanic plume over Io

27 usly undetected H ILyman-alpha emission from Io were obtained with the Hubble space telescope imaging

28 has detected diffuse optical emissions from Io in high-resolution images acquired while the satellit

29 en in the trace gas sodium observed far from Io.

30 these atoms originate in volcanic gases from Io, undergo significant evolution through various electr

31 ervations, a large outburst of material from Io-inferred to be caused by the eruption of a volcanic p

32 If Io has a shallow global magma ocean, its tidal deformati

33 confirm that a shallow global magma ocean in Io does not exist and are consistent with Io having a mo

34 re lavas hint at a global magma reservoir in Io, but no direct evidence has been available.

35 on the dynamo dipolar field generated inside Io.

36 This study provides insights into Io-genic plasma transport at Jupiter and the unique role

37 ynamics support nonballistic models of large Io plumes and also suggest that most visible plume parti

38 the alternative commuting strategy for many 'Io represents a cryptic movement pattern in the species,

39 hotopolarimeter-radiometer instrument mapped Io's thermal emission during the I24, I25, and I27 flyby

40 ft's radio carrier wave were used to measure Io's external gravitational field.

41 Voyager stereoimages of Euboea Montes, Io, indicate that this mountain formed when a large crus

42 The Jovian moon Io hosts the most powerful persistently active volcano i

43 Jupiter's moon Io hosts extensive volcanism, driven by tidal heating.

44 Jupiter's moon Io is known to host active volcanoes.

45 On Jupiter's moon Io, volcanic plumes and evaporating lava flows provide h

46 rough interactions with plasma from the moon Io inside its magnetic field (although other processes f

47 d spectral images of Jupiter's volcanic moon Io, acquired during the October and November 1999 and Fe

48 a source of ions as Jupiter's volcanic moon Io.

49 nt to that associated with the volcanic moon Io.

50 ation on Jupiter's volcanically active moon, Io, has to date been attributed almost exclusively to la

51 The innermost Galilean moon, Io, exhibits widespread tidally-driven volcanism.

52 netary atmospheres, such as the Jovian moons Io, Europa, and Ganymede.

53 he Laplace resonance linking Jupiter's moons Io, Europa and Ganymede.

54 nces in our understanding of Jupiter's moons Io, Europa, Ganymede, and Callisto over the past few yea

55 produced deep inside the magnetosphere near Io's orbit to escape in the antisolar direction down the

56 ata collected by the Galileo spacecraft near Io provide evidence of electromagnetic induction from a

57 sion was seen from individual volcanoes near Io's sub-Jupiter and anti-Jupiter points.

58 The New Horizons (NH) spacecraft observed Io's aurora in eclipse on four occasions during spring 2

59 March 2015 ut as the limb of Europa occulted Io.

60 The isotopic composition of Io's inventory of volatile chemical elements, including

61 ization of S2 gas is a widespread feature of Io volcanism.

62 Plasma measurements made during the flyby of Io on 7 December 1995 with the Galileo spacecraft plasma

63 getic particles detector during the flyby of Io.

64 ing from the electromagnetic interactions of Io, Europa, and Ganymede with the magnetospheric plasma

65 ly passed directly through the ionosphere of Io.

66 Here we report the measurement of Io's tidal deformation, quantified by the gravitational

67 Infrared wavelength observations of Io by the Galileo spacecraft show that at least 12 diffe

68 We used submillimeter observations of Io's atmosphere to measure sulfur isotopes in gaseous su

69 high-energy particles from near the orbit of Io to probe entry into the jovian atmosphere.

70 ss with a radius that is about 52 percent of Io's mean radius of 1821.3 kilometers; if the core is pu

71 t depth induced during vertical recycling of Io's crust.

72 ow appears concentrated on the night side of Io, possibly produced by atomic sodium.

73 Comparisons to detailed simulations of Io's aurora indicate that volcanoes supply 1 to 3% of th

74 ons spacecraft obtained a global snapshot of Io's volcanism.

75 Some of Io's plasma is captured by the planet's strong magnetic

76 Spectroscopy of Io's Pele plume against Jupiter by the Hubble Space Tele

77 ) are the mean orbital angular velocities of Io, Europa, and Ganymede, respectively.

78 xtends well beyond the immediate vicinity of Io's flux-tube interaction with Jupiter, and much farthe

79 Mountain formation on Io may involve localized deep-rooted thrust faulting and

80 everal active volcanic regions were found on Io, with temperatures of 420 to 620 kelvin and projected

81 aused by the eruption of a volcanic plume on Io-caused a transient increase in the neutral cloud and

82 orphology reveals the influence of plumes on Io's electrodynamic interaction with Jupiter's magnetosp

83 ry of high-temperature silicate volcanism on Io, discovery of tenuous oxygen atmospheres at Europa an

84 the longevity of the extensive volcanism on Io, may explain a liquid ocean on Europa, and may guide

85 Diffuse red deposits near other Io volcanoes suggest that venting and polymerization of

86 ropa in eclipse, a giant volcanic plume over Io's north pole, disk-resolved images of the satellite H

87 ot NFATc1, NFATc2, or NFATc4, attenuated PMA/Io-induced REDD1 expression.

88 RNA and protein expression and increased PMA/Io-mediated REDD1 promoter activity.

89 Treatment with PMA/Io increased expression of the goblet cell differentiati

90 Treatment with PMA/Io increased REDD1 promoter activity and increased NFATc

91 field, in contrast to Ganymede and possibly Io.

92 the interaction of Jupiter and its satellite Io extend to a surprisingly high altitude, indicating lo

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

94 r structure of the four galilean satellites--Io, Europa, Ganymede and Callisto-ranged from uniform mi

95 's magnetic field and the plasma surrounding Io, driving currents of around 1 million amperes down th

96 igh, about an order of magnitude dimmer than Io's footprint and below the observable threshold, consi

97 by Io because its gyroradius is smaller than Io's diameter.

98 Now it appears that Io has a large metallic core and that Ganymede is strong

99 netic field, without the need to assume that Io has a magnetized interior.

100 field is consistent with the assumption that Io is in tidal and rotational equilibrium.

101 These results indicate that Io has been volcanically active for most (or all) of its

102 erage Solar System values and indicates that Io has lost 94 to 99% of its available sulfur.

103 and 1999 trajectories crossed, we infer that Io's exosphere is temporally variable.

104 It seems plausible that Io, like Earth and Mercury, is a magnetized solid planet

105 However, recent observations show that Io does not have one.

106 We also show that Io's magnetic footprint extends well beyond the immediat

107 pulsations that propagate rapidly along the Io footprint tail.

108 A 6-month-long monitoring campaign of the Io plasma torus and neutral cloud was conducted to deter

109 that ejects sodium only from the wake of the Io-torus interaction, together with a visually distinct,

110 d-aligned electron beams associated with the Io-Jupiter coupling, for example, create an auroral foot

111 The 'Io is a forest adapted Buteo but occurs across a diverse

112 ckground jovian field at closest approach to Io, was recorded.

113 about 500 Jupiter radii, and a jet close to Io.

114 Moreover, SO+ emissions were seen closer to Io than SO2+ emissions, suggesting that the exosphere wa

115 October 1999, Galileo passed even closer to Io, this time across the upstream side relative to the f

116 onal field which reveal that, in contrast to Io and Ganymede, this galilean satellite is most probabl

117 dense plasma that is at rest with respect to Io.

118 te the relative contribution of volcanoes to Io's atmosphere and its interaction with Jupiter's magne

119 iolet emission that remains fixed underneath Io as Jupiter rotates.

120 Three distinct components make up Io's visible emissions.

121 in Io does not exist and are consistent with Io having a mostly solid mantle(2).

122 generated by its dynamical interaction with Io and Ganymede, which should cause the equilibrium spin

123 nd Saturn like that which links Jupiter with Io, Europa and Ganymede.

124 produce a banana-shaped cloud orbiting with Io, a giant nebula extending out to about 500 Jupiter ra

125 The amount of tidal energy dissipated within Io is enormous and has been suggested to support the lar