Astronomy and Astrophysics – Astrophysics
Scientific paper
Aug 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd..12e..25o&link_type=abstract
Long Wavelength Astrophysics, 26th meeting of the IAU, Joint Discussion 12, 21 August 2006, Prague, Czech Republic, JD12, #25
Astronomy and Astrophysics
Astrophysics
Scientific paper
The purpose of this work is to develop the research technique of the thin structure of outer solar wind in decameter waves. The extended medium model and Feynman path-integral method were applied for calculations of the cross - spectra of weak interplanetary scintillations. The temporary spectra W(f) and phase speed dispersion dependencies V(f) for the spherically symmetric (curves 1) and two-high-speed (curves 2) models of solar wind were calculated. The meanings of solar wind parameters were chosen so that the differences of temporary spectra for two models were minimal and laid within the limits of probable measurements errors ([S:f:S][Author ID2: at Fri Jul 14 10:28:00 2006 ] F[Author ID2: at Fri Jul 14 10:28:00 2006 ]ig. 1). It is shown that the supervision of scintillations on two spatially carried antennas and study of dispersion dependence of phase speed will allow to notice the presence of the accelerated flows on a beam of sight when the measurements on one antenna do not give the unequivocal answer to the question whether the flows of solar wind with various speeds are present in external areas of interplanetary medium. It is shown that by using of simultaneous measurements of temporary spectra and dispersion dependences of phase speed the detection of fast and slow solar wind flows and the definition of their parameters are possible in decameter radio waves.
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