Lunar surface magnetic fields and their interaction with the solar wind: Results from lunar prospector

Science

Volumn 281, Issue 5382, 1998, Pages 1480-1484

  Lin, R P ^a   Mitchell, D L ^a   Curtis, D W ^a   Anderson, K A ^a   Carlson, C W ^a   McFadden, J ^a   Acuna M H ^b   Hood, L L ^c   Binder, A ^d  

^a UNIVERSITY OF CALIFORNIA   (United States)

^b NASA GODDARD SPACE FLIGHT CENTER   (United States)

^c UNIVERSITY OF ARIZONA   (United States)

^d Lunar Research Institute   (United States)

Author keywords

[No Author keywords available]

Indexed keywords

ARTICLE; GEOLOGY; MAGNETIC FIELD; MOON; PRIORITY JOURNAL; REFLECTOMETRY; SOLAR RADIATION; SPACE FLIGHT;

EID: 0032483455     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.281.5382.1480     Document Type: Article

References (44)

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13. There is some evidence that the virtual geomagnetic poles of these regions (the direction of the magnetic south pole of the moon-centered dipole that accounts for the observed crustal magnetic field) cluster around three axes. Changes in the global dipole orientation may have been caused by dynamo field reversals and reorientation of the moon's spin axis by giant impacts, although this interpretation is controversial [S. K. Runcorn, Proc. Lunar Planet. Sci. Conf. 11, 1867 (1980); Phys. Earth Planet. Int. 29, 135 (1982); L. L. Hood, Proc. Lunar Planet. Sci. Conf. 12, 817 (1981)].
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15. There is some evidence that the virtual geomagnetic poles of these regions (the direction of the magnetic south pole of the moon-centered dipole that accounts for the observed crustal magnetic field) cluster around three axes. Changes in the global dipole orientation may have been caused by dynamo field reversals and reorientation of the moon's spin axis by giant impacts, although this interpretation is controversial [S. K. Runcorn, Proc. Lunar Planet. Sci. Conf. 11, 1867 (1980); Phys. Earth Planet. Int. 29, 135 (1982); L. L. Hood, Proc. Lunar Planet. Sci. Conf. 12, 817 (1981)].
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44. The contributions of P. Turin, R. Ulrich, R. Sterling, and J. Scheifele to the development of the experiment and data processing system are gratefully acknowledged. D.L.M. acknowledges discussions with S. D. Bale. WIND data were obtained from the Solar Wind Experiment (K. W. Olgilvie) and Magnetic Fields Investigation (R. P. Lepping) key parameter files. Research at the University of California, Berkeley, was supported by NASA through subcontract LMSC-HG80E477OR from Lockheed-Martin.