Abstract

Abstract. Noon foF2 monthly median values for equinoctial months of solar cycles 20, 21 and 22, were analyzed for 37 worldwide stations. For each solar cycle and for a given Rz, the difference between foF2 in the falling branch of the cycle and the corresponding value of the rising branch is evaluated. The maximum difference, considered as the hysteresis magnitude, varies systematically with geomagnetic latitude. The pattern is similar for every cycle, with greater hysteresis magnitudes for stronger solar cycles. It is positive between 45° S and 45° N, with minimum values at equatorial latitudes and maximum at around 25°–30° on either side of the equator. For latitudes greater than 50° negative values are observed. At around 25°–30° and at high latitudes the hysteresis magnitude reaches 2 MHz for solar cycle with high activity levels, which represents around 20% of foF2. The effects of foF2 hysteresis on the analysis of long-term data sequences is analyzed. In the case of long-term trend analysis, the hysteresis behavior may induce spurious trends as a consequence of the filtering processes applied to foF2 time series previous to trend values estimation. This problem may be solved by considering time series covering several solar cycles.

Highlights

  • The F2 critical frequency foF2, for a given station and a constant value of the solar activity level, such as the sunspot number Rz, can differ for the rising and falling parts of the 11-year solar cycle

  • In our case, negative values at high latitudes are as important as the positive values around mid-latitudes

  • The latitudinal pattern of the hysteresis magnitude is similar in shape to that of foF2 diurnal mean values, which shows a pronounced trough at the magnetic equator and crests at about 30◦ N and 30◦ S magnetic dip

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Summary

Introduction

The F2 critical frequency foF2, for a given station and a constant value of the solar activity level, such as the sunspot number Rz, can differ for the rising and falling parts of the 11-year solar cycle. For each solar cycle and for a given Rz, the difference between foF2 in the falling branch of the cycle and the corresponding value of the rising branch is evaluated.

Results
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