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Far-Ultraviolet Imaging Spectroscopy of Io's Atmosphere with HST/STIS

Science
15 Jan 1999
Vol 283, Issue 5400
pp. 353-357

Abstract

Well-resolved far-ultraviolet spectroscopic images of Oi, S i, and previously undetected H iLyman-α emission from Io were obtained with the Hubble space telescope imaging spectrograph (STIS). Detected O i and Si lines (1250 to 1500 angstroms) have bright equatorial spots (up to 2.5 kilorayleighs) that shift position with jovian magnetic field orientation; limb glow that is brighter on the hemisphere facing the jovian magnetic equator; and faint diffuse emission extending to ∼20 Io radii. All O i and Si features brightened by ∼50 percent in the last two images, concurrently with a ground-based observation of increased iogenic [O i] 6300-angstrom emission. The H iLyman-α emission, consisting of a small, ∼2-kilorayleigh patch near each pole, has a different morphology and time variation.

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REFERENCES AND NOTES

1
Scherb F., Smyth W. H., J. Geophys. Res. 98, 18729 (1993).
2
J. T. Trauger, K. R. Stapelfeldt, G. E. Ballester, J. T. Clarke, WFPC2 Science Team, Bull. Am. Astron. Soc. 29, 1002 (1997).
3
Ballester G. E., et al., Astrophys. J. 319, L33 (1987).
4
Ballester G. E., et al., Bull. Am. Astron. Soc. 29, 980 (1997).
5
Clarke J. T., Ajello J., Luhmann J., Schneider N. M., Kanik I., J. Geophys. Res. 99, 8387 (1994).
6
Durrance S. T., et al., Astrophys. J. 447, 408 (1995).
7
Fox G. K., et al., Astronom. J. 113, 1158 (1997);
Sandel B. R., Broadfoot A. L., J. Geophys. Res. 87, 212 (1982);
Spencer J. R., Schneider N. M., Annu. Rev. Earth Planet. Sci. 24, 125 (1996).
8
B. E. Woodgate et al., Proc. Astron. Soc. Pacific 110, 1183 (October 1998).
9
Kimble R. A., et al., Astrophys. J. 492, L83 (1998).
10
In time-tag mode, each photon's arrival time and position in the STIS multi-anode microchannel array (MAMA) are recorded individually.
11
M. Voit, Ed., HST Data Handbook (Space Telescope Science Institute, Baltimore, ed. 3.0, 1997).
12
The slit was effectively reduced to 30 arc sec by 2 arc sec (September) and 25 arc sec by 2 arc sec (October) by the finite size of the MAMA detectors.
13
The STIS is equipped with two MAMAs, which have different photocathodes sensitive to different wavelength ranges (8). Unfortunately, the NUV MAMA (covering 1650 to 3100 Å) was found after launch to have a dark rate exceeding design specification by about an order of magnitude, as a result of excessive phosphoresence in its MgF2 window (9). Consequently, our G230M data (orbits 1 and 2) are noisy, and only the brightest features can be distinguished; these data are largely excluded from this paper.
14
It is unclear whether the near-Io emission at ∼1250 Å is predominately S i λ1251 or S ii λ1256.
15
McEwen A. S., et al., Geophys. Res. Lett. 24, 2443 (1997).
16
Smith T. E., McGrath M. A., Sartoretti P., Bull. Am. Astron. Soc. 27, 1157 (1995).
17
G. E. Ballester et al., in Magnetospheres of the Outer Planets (Boulder, CO, March 1997), unpublished proceedings.
18
One Rayleigh is 106 photons 4π sr−1 cm−2 s−1.
19
Io's electrodynamic interaction with the plasma torus is typical of plasma flowing past an obstacle. In this case it is sub-Alfvénic (vplasma ∼ 57 km/s, vA ∼ 300 km/s), with no bowshock forming and standing magnetohydrodynamic Alfvén waves in Io's rest frame. The corotational electric field of 0.114 V/m produces a ∼400-kV voltage drop across Io, driving a current of a few million amperes through Io's ionosphere; Alfvén waves carry the current along the essentially equipotential magnetic field lines into Io's inner hemisphere and away from its outer hemisphere. (Electrons, the likely current carriers, would of course flow in the opposite direction.) The current loop can be completed in Jupiter's ionosphere only if the round trip travel time for an Alfvén wave is short compared with the time it takes for torus plasma to sweep past Io; otherwise, the current loop is closed in the plasma torus (45).
20
J. Saur, F. M. Neubauer, D. F. Strobel, M. E. Summers, in preparation.
21
Kivelson M. G., et al., Science 273, 337 (1996);
Kivelson M. G., et al., ibid. 274, 396 (1996).
22
Geissler P. E., et al., Bull. Am. Astron. Soc. 30, 1116 (1998).
23
McEwen A. S., et al., Icarus 135, 181 (1998).
24
Jupiter's magnetic equator is tilted 9.6° with respect to its spin equator and Io's orbital plane. Jupiter's centrifugal equator—the locus of points that, of all points on a magnetic field line, are the farthest from Jupiter's spin axis—lies between the magnetic and spin equators. The Io plasma torus is densest at, and approximately symmetric about, the centrifugal equator.
25
Woodward R. C., Smyth W. H., Bull. Am. Astron. Soc. 26, 1139 (1994).
26
Frank L. A., et al., Science 274, 394 (1996).
27
Bagenal F., et al., Geophys. Res. Lett. 24, 2119 (1997).
28
Oliversen R. J., et al., Bull. Am. Astron. Soc. 29, 1315 (1997).
29
Scherb F., Retherford K. D., Woodward R. C., Smyth W. H., ibid. 28, 1155 (1996).
30
Judge D. L., Carlson R. W., Science 183, 317 (1974).
31
Wu F. M., Gangopadhyay P., Judge D. L., J. Geophys. Res. 100, 3481 (1995).
32
The terrestrial glow still contributed significant photon noise to our data, especially because we made these observations 2 months after opposition, and a fraction of the Earth's exosphere along our line of sight was therefore sunlit. This effect was most pronounced at the beginning of each orbit.
33
Lellouch E., Icarus 124, 1 (1996).
34
No correction has been made for the fact that Io blocks part of the H i Lyman-α emission from the interplanetary medium; all Io H i Lyman-α intensities given in this research article could therefore be 200 to 900 Rayleighs too low. Fluxes given in row 2 of Table 3 are not subject to this correction.
35
Nash D. B., Howell R. R., Science 244, 454 (1989).
36
McEwen A. S., Johnson T. V., Matson D. L., Soderblom L. A., Icarus 75, 450 (1988).
37
Lellouch E., et al., ibid. 98, 271 (1992).
38
F. Salama et al., ibid. 107, 413 (1994);
Carlson R. W., et al., Geophys. Res. Lett. 24, 2479 (1997).
39
Williams D. J., et al., Science 274, 401 (1996).
40
Spencer J. R., Schneider N. M., Annu. Rev. Earth Planet. Sci. 24, 125 (1996).
41
Manatt S. A., Lane A. L., J. Quant. Spectrosc. Radiat. Transfer 50, 267 (1993).
42
Wong M. C., Johnson R. E., J. Geophys. Res. 101, 23243 (1996).
43
Chust T., Roux A., Perraut S., Gurnett D. A., Ann. Geophys. 15, C824 (1997).
44
Frank L. A., Paterson W. R., Ackerson K. L., Bolton S. J., Eos 79, S201 (1998).
45
Wolf-Gladrow D. A., Neubaer F. M., Lussem M., J. Geophys. Res. 92, 9949 (1987).
46
We thank D. Hall for valuable assistance in planning this experiment, and J. Corliss and M. Freed for long hours spent in data reduction. We also gratefully acknowledge the cooperation and assistance of our co-workers on the STIS Instrument Development Team, and the many people at the Space Telescope Science Institute whose work made these observations possible. We thank anonymous reviewers for valuable comments on the manuscript. A portion of D.F.S.'s research was accomplished at the Observatoire de Paris-Meudon; he thanks Département de Recherche Spatiale for its hospitality. This work was supported by NASA grants NAGW-3319, NAG-4168, and NAGW-6546, and NASA contracts NAS5-30131 and NAS5-30403.

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Published In

Science
Volume 283 | Issue 5400
15 January 1999

Submission history

Received: 24 August 1998
Accepted: 10 December 1998
Published in print: 15 January 1999

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Authors

Affiliations

F. L. Roesler
F. L. Roesler, R. C. Woodward Jr., and F. Scherb are in the Physics Department, University of Wisconsin, 1150 University Avenue, Madison, WI 53706, USA. H. W. Moos, K. D. Retherford, and P. D. Feldman are in the Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA. R. J. Oliversen is in the Laboratory for Astronomy and Solar Physics, NASA–Goddard Space Flight Center, Greenbelt, MD 20771, USA. M. A. McGrath is at the Space Telescope Science Institute, Baltimore, MD 21218, USA. W. H. Smyth is with Atmospheric and Environmental Research, Cambridge, MA 02139, USA. D. F. Strobel is in the Department of Earth and Planetary Science, Johns Hopkins University, Baltimore, MD 21218, USA.
H. W. Moos
F. L. Roesler, R. C. Woodward Jr., and F. Scherb are in the Physics Department, University of Wisconsin, 1150 University Avenue, Madison, WI 53706, USA. H. W. Moos, K. D. Retherford, and P. D. Feldman are in the Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA. R. J. Oliversen is in the Laboratory for Astronomy and Solar Physics, NASA–Goddard Space Flight Center, Greenbelt, MD 20771, USA. M. A. McGrath is at the Space Telescope Science Institute, Baltimore, MD 21218, USA. W. H. Smyth is with Atmospheric and Environmental Research, Cambridge, MA 02139, USA. D. F. Strobel is in the Department of Earth and Planetary Science, Johns Hopkins University, Baltimore, MD 21218, USA.
R. J. Oliversen
F. L. Roesler, R. C. Woodward Jr., and F. Scherb are in the Physics Department, University of Wisconsin, 1150 University Avenue, Madison, WI 53706, USA. H. W. Moos, K. D. Retherford, and P. D. Feldman are in the Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA. R. J. Oliversen is in the Laboratory for Astronomy and Solar Physics, NASA–Goddard Space Flight Center, Greenbelt, MD 20771, USA. M. A. McGrath is at the Space Telescope Science Institute, Baltimore, MD 21218, USA. W. H. Smyth is with Atmospheric and Environmental Research, Cambridge, MA 02139, USA. D. F. Strobel is in the Department of Earth and Planetary Science, Johns Hopkins University, Baltimore, MD 21218, USA.
R. C. Woodward, Jr.*
F. L. Roesler, R. C. Woodward Jr., and F. Scherb are in the Physics Department, University of Wisconsin, 1150 University Avenue, Madison, WI 53706, USA. H. W. Moos, K. D. Retherford, and P. D. Feldman are in the Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA. R. J. Oliversen is in the Laboratory for Astronomy and Solar Physics, NASA–Goddard Space Flight Center, Greenbelt, MD 20771, USA. M. A. McGrath is at the Space Telescope Science Institute, Baltimore, MD 21218, USA. W. H. Smyth is with Atmospheric and Environmental Research, Cambridge, MA 02139, USA. D. F. Strobel is in the Department of Earth and Planetary Science, Johns Hopkins University, Baltimore, MD 21218, USA.
K. D. Retherford
F. L. Roesler, R. C. Woodward Jr., and F. Scherb are in the Physics Department, University of Wisconsin, 1150 University Avenue, Madison, WI 53706, USA. H. W. Moos, K. D. Retherford, and P. D. Feldman are in the Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA. R. J. Oliversen is in the Laboratory for Astronomy and Solar Physics, NASA–Goddard Space Flight Center, Greenbelt, MD 20771, USA. M. A. McGrath is at the Space Telescope Science Institute, Baltimore, MD 21218, USA. W. H. Smyth is with Atmospheric and Environmental Research, Cambridge, MA 02139, USA. D. F. Strobel is in the Department of Earth and Planetary Science, Johns Hopkins University, Baltimore, MD 21218, USA.
F. Scherb
F. L. Roesler, R. C. Woodward Jr., and F. Scherb are in the Physics Department, University of Wisconsin, 1150 University Avenue, Madison, WI 53706, USA. H. W. Moos, K. D. Retherford, and P. D. Feldman are in the Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA. R. J. Oliversen is in the Laboratory for Astronomy and Solar Physics, NASA–Goddard Space Flight Center, Greenbelt, MD 20771, USA. M. A. McGrath is at the Space Telescope Science Institute, Baltimore, MD 21218, USA. W. H. Smyth is with Atmospheric and Environmental Research, Cambridge, MA 02139, USA. D. F. Strobel is in the Department of Earth and Planetary Science, Johns Hopkins University, Baltimore, MD 21218, USA.
M. A. McGrath
F. L. Roesler, R. C. Woodward Jr., and F. Scherb are in the Physics Department, University of Wisconsin, 1150 University Avenue, Madison, WI 53706, USA. H. W. Moos, K. D. Retherford, and P. D. Feldman are in the Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA. R. J. Oliversen is in the Laboratory for Astronomy and Solar Physics, NASA–Goddard Space Flight Center, Greenbelt, MD 20771, USA. M. A. McGrath is at the Space Telescope Science Institute, Baltimore, MD 21218, USA. W. H. Smyth is with Atmospheric and Environmental Research, Cambridge, MA 02139, USA. D. F. Strobel is in the Department of Earth and Planetary Science, Johns Hopkins University, Baltimore, MD 21218, USA.
W. H. Smyth
F. L. Roesler, R. C. Woodward Jr., and F. Scherb are in the Physics Department, University of Wisconsin, 1150 University Avenue, Madison, WI 53706, USA. H. W. Moos, K. D. Retherford, and P. D. Feldman are in the Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA. R. J. Oliversen is in the Laboratory for Astronomy and Solar Physics, NASA–Goddard Space Flight Center, Greenbelt, MD 20771, USA. M. A. McGrath is at the Space Telescope Science Institute, Baltimore, MD 21218, USA. W. H. Smyth is with Atmospheric and Environmental Research, Cambridge, MA 02139, USA. D. F. Strobel is in the Department of Earth and Planetary Science, Johns Hopkins University, Baltimore, MD 21218, USA.
P. D. Feldman
F. L. Roesler, R. C. Woodward Jr., and F. Scherb are in the Physics Department, University of Wisconsin, 1150 University Avenue, Madison, WI 53706, USA. H. W. Moos, K. D. Retherford, and P. D. Feldman are in the Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA. R. J. Oliversen is in the Laboratory for Astronomy and Solar Physics, NASA–Goddard Space Flight Center, Greenbelt, MD 20771, USA. M. A. McGrath is at the Space Telescope Science Institute, Baltimore, MD 21218, USA. W. H. Smyth is with Atmospheric and Environmental Research, Cambridge, MA 02139, USA. D. F. Strobel is in the Department of Earth and Planetary Science, Johns Hopkins University, Baltimore, MD 21218, USA.
D. F. Strobel
F. L. Roesler, R. C. Woodward Jr., and F. Scherb are in the Physics Department, University of Wisconsin, 1150 University Avenue, Madison, WI 53706, USA. H. W. Moos, K. D. Retherford, and P. D. Feldman are in the Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA. R. J. Oliversen is in the Laboratory for Astronomy and Solar Physics, NASA–Goddard Space Flight Center, Greenbelt, MD 20771, USA. M. A. McGrath is at the Space Telescope Science Institute, Baltimore, MD 21218, USA. W. H. Smyth is with Atmospheric and Environmental Research, Cambridge, MA 02139, USA. D. F. Strobel is in the Department of Earth and Planetary Science, Johns Hopkins University, Baltimore, MD 21218, USA.

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