Hydrogen peroxide on the surface of Europa

Science

Volumn 283, Issue 5410, 1999, Pages 2062-2064

  Carlson, R W ^a   Anderson, M S ^a   Johnson, R E ^b   Smythe, W D ^a   Hendrix, A R ^c   Barth, C A ^c   Soderblom, L A ^d   Hansen, G B ^e   McCord, T B ^e   Dalton, J B ^d   Clark, R N ^d   Shirley, J H ^a   Ocampo, A C ^a   Matson, D L ^a  

^a CALIFORNIA INSTITUTE OF TECHNOLOGY   (United States)

^b University of Virginia   (United States)

^c UNIVERSITY OF COLORADO   (United States)

^d U S GEOLOGICAL SURVEY   (United States)

^e UNIVERSITY OF HAWAII   (United States)

Author keywords

[No Author keywords available]

Indexed keywords

HYDROGEN PEROXIDE;

EUROPA; HYDROGEN PEROXIDE; PLANETARY SURFACE;

ARTICLE; ASTRONOMY; ENERGY; INFRARED RADIATION; INFRARED SPECTROMETRY; PRIORITY JOURNAL; RADIOLYSIS; SURFACE PROPERTY; ULTRAVIOLET RADIATION;

NON-PROGRAMMATIC;

EXTRATERRESTRIAL ENVIRONMENT; HYDROGEN PEROXIDE; ICE; JUPITER; SPECTROPHOTOMETRY, INFRARED; SPECTROPHOTOMETRY, ULTRAVIOLET; WATER;

EID: 0033605630     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.283.5410.2062     Document Type: Article

References (44)

1. R. Greeley et al., Icarus 135, 4 (1998).
2. A. L. Lane, R. M. Nelson, D. L. Matson, Nature 292, 38 (1981).
3. M. E. Brown and R. E. Hill, ibid. 380, 229 (1996).
4. W. H. Ip, D. J. Williams, R. W. McEntire, B. H. Mauk, Geophys. Res. Lett. 25, 829 (1998).
5. R. E. Johnson, Energetic Charged-particle Interactions with Atmospheres and Surfaces (Springer-Verlag, Berlin, 1990).
6. R. E. Johnson and T. I. Quickenden, J. Geophys. Res. 102, 10985 (1997).
7. W. M. Calvin, R. N. Clark, R. H. Brown, J. R. Spencer, ibid. 100, 19041 (1995).
8. K. S. Noll, H. A. Weaver, A. M. Gonella, ibid., p. 19057.
9. T. B. McCord et al., Science 280, 1242 (1998); T. B. McCord et al., J. Geophys. Res., in press.
10. T. B. McCord et al., Science 280, 1242 (1998); T. B. McCord et al., J. Geophys. Res., in press.
11. R. E. Johnson, R. M. Killen, J. H. Waite, W. S. Lewis, Geophys. Res. Lett. 25, 3257 (1998).
12. M. H. Carr et al., Nature 391, 363 (1998).
13. R. W. Carlson et al., Space Sci. Rev. 60, 457 (1992).
14. W. D. Smythe et al., paper presented at the 29th Lunar and Planetary Science Conference, Houston, TX, 16 to 20 March 1998 (Lunar and Planetary Institute, Houston, TX, 1998).
15. R. Carlson et al., Science 274, 385 (1996); T. B. McCord et al., ibid. 278, 271 (1997); T. B. McCord et al., J. Geophys. Res. 103, 8603 (1998).
16. R. Carlson et al., Science 274, 385 (1996); T. B. McCord et al., ibid. 278, 271 (1997); T. B. McCord et al., J. Geophys. Res. 103, 8603 (1998).
17. R. Carlson et al., Science 274, 385 (1996); T. B. McCord et al., ibid. 278, 271 (1997); T. B. McCord et al., J. Geophys. Res. 103, 8603 (1998).
18. C. W. Hord et al., Space Sci. Rev. 60, 503 (1992).
19. The measurements were obtained on 6 November 1997, when Galileo was 480,000 km from Europa. The orbital phase angle and subsolar longitude were 89°, and the subspacecraft longitude was 152°.
20. D. M. Hudgins, S. A. Sandford, L. J. Allamandola, A. Tielens, Astrophys. J. Suppl. 86, 713 (1993).
21. R. N. Clark, G. A. Swayze, A. Gallagher, T. V. V. King, W. M. Calvin, "The U.S. Geological Survey Digital Spectral Library: Version 1: 0.2 to 3.0 μm," U.S. Geological Survey Open File Report 93-592.
22. O. Bain and P. A. Giguere, Can. J. Chem. 33, 527 (1955); R. L Miller and D. F. Hornig, J. Chem. Phys. 34, 265 (1961).
23. O. Bain and P. A. Giguere, Can. J. Chem. 33, 527 (1955); R. L Miller and D. F. Hornig, J. Chem. Phys. 34, 265 (1961).
24. P. A. Giguere and K. B. Harvey, J. Mol. Spectrosc. 3, 36 (1959).
25. 2 abundance is estimated to be: ±50.
26. P. A. Gerakines, W. A. Schutte, P. Ehrenfreund, Astron. Astrophys. 312, 289 (1996).
27. We adopt, for the effective penetration depth, that level for which the optical depth for equivalent isotropic scatterers is unity. Using similarity relations [B. Hapke, Theory of Reflectance and Emittance Spectroscopy (Cambridge Univ. Press, Cambridge, 1993), p. 197] with computed single-scattering albedos and asymmetry parameters (25), we find penetration depths for a nonporous medium of 60-μm ice grains of about 60, 250, and 500 μm for wavelengths of 3.5 μm, 210 nm, and 300 nm, respectively.
28. The reflectance factor is the ratio of the observed radiance to that of a perfectly diffuse plane reflector illuminated at the same geometry [B. Hapke (23), p. 262].
29. R. W. Carlson and T. Arakelian [Antarctic J. U. S. 28, 256 (1993)] outline the computational method. We used UV and IR optical constants from S. G. Warren [Appl. Opt. 23, 1206 (1984)] and J. E. Bertie, H. J. Labbe, and E. Whalley [J. Chem. Phys. 50, 4501 (1969)], respectively.
30. R. W. Carlson and T. Arakelian [Antarctic J. U. S. 28, 256 (1993)] outline the computational method. We used UV and IR optical constants from S. G. Warren [Appl. Opt. 23, 1206 (1984)] and J. E. Bertie, H. J. Labbe, and E. Whalley [J. Chem. Phys. 50, 4501 (1969)], respectively.
31. R. W. Carlson and T. Arakelian [Antarctic J. U. S. 28, 256 (1993)] outline the computational method. We used UV and IR optical constants from S. G. Warren [Appl. Opt. 23, 1206 (1984)] and J. E. Bertie, H. J. Labbe, and E. Whalley [J. Chem. Phys. 50, 4501 (1969)], respectively.
32. C. L. Lin, N. K. Rohatgi, W. B. DeMore, Geophys. Res. Lett. 5, 113 (1978).
33. A. R. Hendrix, C. A. Barth, C. W. Hord, A. L. Lane, Icarus 135, 79 (1998).
34. Samples 3 mm thick were frozen, forming granular, diffusing surfaces. The diffuse reflectance was measured, avoiding specular reflection. The UV and IR laboratory measurements were performed at the JPL Vibrational Spectroscopy Laboratory with the use of an Analect diffuse-reflectance attachment with Bio-Rad FTS 6000 and Cary 5E spectrometers.
35. -4 M data from (26) were used.
36. M. T. Sieger, W. C. Simpson, T. M. Orlando, Nature 394, 554 (1998).
37. We used electron and ion fluxes (for an unmagnetized body at Europa's orbit) and stopping depths in ice from J. F. Cooper, R E. Johnson, B. H. Mauk, and N. Gehrels (Icarus, in preparation). Ion fluxes were increased by a factor of 2 for the finite gyroradius effect (4).
38. M. Cottin and M. Lefort, J. Chim. Phys. 52, 545 (1955). Measurements for other particles are needed.
39. W. F. Huebner, J. J. Keady, S. P. Lyon, Astrophys. Space Sci. 195, 1 (1992).
40. J. A. Ghormley and A. C. Stewart, J. Am. Chem. Soc. 78, 2934 (1956).
41. R. Schriever, M. Chergui, N. Schwentner, J. Phys. Chem. 95, 6124 (1991).
42. D. T. Hall, D. F. Strobel, P. D. Feldman, M. A. McGrath, H. A. Weaver, Nature 373, 677 (1995).
43. D. L Domingue and A. L. Lane, Geophys. Res. Lett. 25, 4421 (1998).
44. Portions of the work described herein were performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract to the National Aeronautics and Space Administration.