Variations of Parameters of the Solar Wind Stream Structure at the Distances More than 1 AU in 2003-2004.

Details Variations of Parameters of the Solar Wind Stream Structure at the Distances More than 1 AU in 2003-2004. Variations of Parameters of the Solar Wind Stream Structure at the Distances More than 1 AU in 2003-2004.

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd..12e..26f&link_type=abstract

Long Wavelength Astrophysics, 26th meeting of the IAU, Joint Discussion 12, 21 August 2006, Prague, Czech Republic, JD12, #26

Astronomy and Astrophysics

Astrophysics

Scientific paper

During 2003-2004 we observed the scintillations of the small size sources at the large solar elongations () with the largest in the world decameter radio telescope UTR-2 equipped with new wide-band radiometers. These allow us to obtain scintillation power spectra with dynamic range of 3 to 4 orders unachievable before at decameter wavelengths. To derive the solar wind parameters, the observed spectra are usually fitted with theoretical ones. For this purpose the phase screen model was frequently used earlier at the high frequencies. However, at the large elongations and decameter wavelengths the scattering medium is essentially expanded, the most scattering layer is situated near an observer, so a multiple scattering theory needs to be used. We adapted and employed the Feynman path-integral technique for the interpretation of the observed power spectra. Then, we built the histograms of the base solar wind parameters for convenience. The brief results of the observations. 1. In 2003 in most cases we observed two solar wind streams along the line of sight: the slow one with the typical velocity of 450 ± 50 km/s, the spectral index of 3.7, the effective thickness ≈ 5 A.U. and the fast one with the typical velocity of 800 ± 50 km/s, the spectral indexes of 3.7 ± 0.2 or 3.4 ± 0.2 and the effective thicknesses of 1.3 or 0.8 AU. Two values of the spectral index and thickness of the fast streams mentioned above are connected with two types of the interplanetary disturbances - transient and corotating shock waves. The velocity and thickness distributions match with those derived from SOHO and other authors' measurements for this period. 2. In 2004 year the observed spectra were described by the two-stream model only in 50% of cases. This fact owes to decreasing the solar activity during the period from 2003 to 2004. 3. In February 2003 we managed to observe the fast stream movement from the large coronal hole in Northern hemisphere of the Sun across the line of sight to the quasar 3C254. The solar wind velocity variations obtained by IPS were compared with those observed on SOHO.

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