Drift of the ionosphere at high latitude determined from radio star scintillations

Details Drift of the ionosphere at high latitude determined from radio star scintillations Drift of the ionosphere at high latitude determined from radio star scintillations

Mar 1963

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1963jatp...25..109h&link_type=abstract

Journal of Atmospheric and Terrestrial Physics, vol. 25, no. 3, pp. 109-119

Physics

Scientific paper

Drift measurements of the irregularities causing scintillations have been made using the Mitra method of similar fades at the Arctic station Tromsö (70°N) lying close to the auroral zone. The radio noise emission 6rom the Cassiopeia source on 45 Mc/s has been recorded simultaneously at three points lying in the corners of a right-angled triangle with bases equal to 600 m. The time delays, Tx and Ty, representing drifts components in the E-W and N-Sdirections were recorded around upper and lower culminations of the radio source for a period covering about half a year. It is shown that the sidereal variation of Tx and Ty is determined by the hour of upper and lower culmination of the radio source, which at Tromsö also coincides with the time of passage across the geomagnetic meridian. The time delays Ty corresponding to the N-S drift component are considerably greater than the Tx-values, and the direction of the N-S component reverses when the radio source crosses the N-S (or geomagnetic) meridian. The Tx-values corresponding to the E-W drift component have median values which always indicate a drift towards W of a magnitude of 400-600 m/s. It is shown that the characteristic reversal of the N-S component is explained if a uniform drift towards W is assumed, and that the diffraction pattern on the ground consists of strongly elongated ellipses with their major axis directed along the projections of the geomagnetic field lines seen from the radio source. The hypothesis put forward by Spencer that the scintillations are due to elongated blobs aligned along the geomagnetic fields is thus supported. It is pointed out that the uniform drift towards W of the region in 350-500 km height causing the scintillations is in accordance with the point of view of a non-rotating upper part of the polar ionosphere.

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