The latitudinal distribution of solar wind magnetic holes

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Abstract

Using the fast latitude scan period of the Ulysses spacecraft, the occurrence of magnetic holes in the solar wind is investigated from -80° to +80° helio-latitude. Near the ecliptic, the large average value and the large variations of the hole count rate appear to be correlated with interaction regions. It is found, however, that at 30°north and south latitude, approximately, the hole count rate drops to about 10% of that in the low latitude region and stays constant at this level to near the poles. The small but non-zero hole count rate at high helio-latitudes indicates that these holes were formed by processes other than the large scale dynamic solar wind features operating in the ecliptic region. Copyright 2000 by the American Geophysical Union.

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Winterhalter, D., Smith, E. J., Neugebauer, M., Goldstein, B. E., & Tsurutani, B. T. (2000). The latitudinal distribution of solar wind magnetic holes. Geophysical Research Letters, 27(11), 1615–1618. https://doi.org/10.1029/1999GL003717

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