Latitudinal dependence of the interplanetary magnetic field spectrum

Details Latitudinal dependence of the interplanetary magnetic field spectrum Latitudinal dependence of the interplanetary magnetic field spectrum

Oct 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987angeo...5..265b&link_type=abstract

Annales Geophysicae, Series A - Upper Atmosphere and Space Sciences (ISSN 0980-8752), vol. 5, Oct. 1987, p. 265-272.

Physics

2

Interplanetary Magnetic Fields, Latitude, Power Spectra, Solar Wind, Current Sheets, Density Distribution, Magnetic Signatures, Spectral Signatures

Scientific paper

Magnetic field data of Helios 1 in 1975 and Helios 2 in 1976 have been used to investigate the dependence of the interplanetary magnetic field power spectrum upon the angular displacement from the magnetic equator. At low wave numbers the magnetic field convected by the slow solar wind (associated to low latitudes) has spectral signatures different from those of the fast wind (associated to high latitudes). Close to the current sheet a spectrum as 1/k is seen, whereas at high latitudes an almost flattened spectrum is found. Power levels are of a factor two higher at low latitudes. All this indicates that, in conditions of low solar activity, interplanetary structures with sizes greater than a few millions of kilometers tend to disappear at high latitudes. A completely different situation is found at high wave numbers, where well developed turbulent spectra (k exp -5/3) with no dependence on latitude are observed. A discussion of these results in terms of the existing models on generation and evolution of the solar wind fluctuations is given.

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