Effects of absorption by Io on composition of energetic heavy ions

Science

Volumn 274, Issue 5286, 1996, Pages 393-394

  Garrard, T L ^a   Stone, E C ^a   Murphy, N ^b  

^a CALIFORNIA INSTITUTE OF TECHNOLOGY   (United States)

^b CALIFORNIA INSTITUTE OF TECHNOLOGY   (United States)

Author keywords

[No Author keywords available]

Indexed keywords

CARBON; IRON; MAGNESIUM; OXYGEN; SILICON;

ABSORPTION; ARTICLE; ASTRONOMY; ENERGY; IONIZATION; MAGNETIC FIELD; PRIORITY JOURNAL; SPACE; TELECOMMUNICATION;

FLIGHT EXPERIMENT; GALILEO PROJECT; LONG DURATION; UNMANNED;

CARBON; EXTRATERRESTRIAL ENVIRONMENT; IONS; JUPITER; NEON; OXYGEN; SODIUM; SULFUR;

EID: 0029852515     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.274.5286.393     Document Type: Article

References (13)

1. S. M. Krimigis et al., Science 204, 998 (1979); R. E. Vogt et al., ibid., p. 1003; S. M. Krimigis et al., ibid. 206, 977 (1979); R. E. Vogt et al., ibid., p. 984.
2. S. M. Krimigis et al., Science 204, 998 (1979); R. E. Vogt et al., ibid., p. 1003; S. M. Krimigis et al., ibid. 206, 977 (1979); R. E. Vogt et al., ibid., p. 984.
3. S. M. Krimigis et al., Science 204, 998 (1979); R. E. Vogt et al., ibid., p. 1003; S. M. Krimigis et al., ibid. 206, 977 (1979); R. E. Vogt et al., ibid., p. 984.
4. S. M. Krimigis et al., Science 204, 998 (1979); R. E. Vogt et al., ibid., p. 1003; S. M. Krimigis et al., ibid. 206, 977 (1979); R. E. Vogt et al., ibid., p. 984.
5. T. L. Garrard, N. Gehrels, E. C. Stone, Space Sci. Rev. 60, 305 (1992).
6. A. Luhn et al., Adv. Space Res. 4, 161 (1984).
7. See, for example, N. Gehrels, E. C. Stone, J. H. Trainor, J. Geophys. Res. 86, 8906 (1981), N. Gehrels, E. C. Stone, ibid. 88, 5537 (1983).
8. See, for example, N. Gehrels, E. C. Stone, J. H. Trainor, J. Geophys. Res. 86, 8906 (1981), N. Gehrels, E. C. Stone, ibid. 88, 5537 (1983).
9. For this report we determined C/O abundance ratios at 8.5 to 11, 11 to 14, 16 to 17, and 31 to 42 MeV per nucleon and S/O abundance ratios at 8.5 to 11, 11 to 14, 14 to 17, 24.7 to 26.24, and 43 to 48 MeV per nucleon.
10. The L value for a drift shell in a centered dipole magnetic field corresponds to the equatorial distance (in planetary radii) of the shell from the center of the planet. The values used here were calculated by C. Paranicas and A. F. Cheng as described in J. Geophys. Res. 99, 19433 (1994).
11. ⊥ is the energy associated with motion perpendicular to the magnetic field and B is the magnetic field strength. M is conserved under radial diffusion.
12. See, for example, T. L. Garrard and E. C. Stone, Proc. 23rd Intl. Cosmic Ray Conf. 3, 364 (1993).
13. This work was supported in part by NASA under NAS7-918.