ライフサイエンスコーパス: Io

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

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

3 ffuse emission extending to approximately 20 Io radii.

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

5 ers per pixel) images of volcanically active Io.

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

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

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

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

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

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

12 ong the trajectory as the spacecraft flew by Io.

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

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

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

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

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

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

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

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

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

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

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

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

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

26 on the dynamo dipolar field generated inside Io.

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

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

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

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

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

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

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

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

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

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

37 nt to that associated with the volcanic moon Io.

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

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

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

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

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

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

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

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

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

47 getic particles detector during the flyby of Io.

48 ly passed directly through the ionosphere of Io.

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

72 field, in contrast to Ganymede and possibly Io.

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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