Comparison of Large-Scale Density Fluctuations in the Outer Corona and in the Inner Heliosphere for Both Fast and Slow Solar Wind

Details Comparison of Large-Scale Density Fluctuations in the Outer Corona and in the Inner Heliosphere for Both Fast and Slow Solar Wind Comparison of Large-Scale Density Fluctuations in the Outer Corona and in the Inner Heliosphere for Both Fast and Slow Solar Wind

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh13b1544t&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SH13B-1544

Other

2164 Solar Wind Plasma, 7509 Corona, 7549 Ultraviolet Emissions, 7811 Discontinuities (2109), 7863 Turbulence (4490)

Scientific paper

The low frequency spectra of the proton density of fast and slow solar wind streams, measured in the inner heliosphere with the HELIOS 2 in-situ instrumentation, are compared with those due to the large-scale density fluctuations observed with the Ultraviolet Coronagraph Spectrometer, UVCS/SOHO, in the outer corona where the streams are accelerated. The interplanetary and coronal data have been detected during solar minimum of different activity cycles. The density fluctuations exhibit the same low-frequency spectral dependence, 1/f2, both in the corona and in the inner heliosphere, thus suggesting that the discontinuities resulting in the 1/f2 noise, observed in the interplanetary space, are likely to have a coronal origin. The present study shows that in the outer corona the fast wind plasma is mainly consisting of Alfvén fluctuations as in the inner heliosphere. Coherent structures, on the other hand, are mainly found in the slow coronal wind. In addition, a high degree of phase synchronization is observed in the slow solar wind fluctuations both at coronal and heliospheric levels. This is an indication that the phase coherent structures observed in the interplanetary medium in the low-speed streams are likely to be advected directly from the acceleration regions of the slow solar wind, rather than resulting as a product of stream-stream dynamic interactions in the heliosphere.

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