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STP12 Abstracts Berlin, 12 - 16 July 2010 SCOSTEP Symposium 2010 The Multi-solar Cycles with Long Periods and Some Extrapolations Tan Baolin Key Laboratory of Solar Activity, National Astronomical Observatories of Chinese Academy of Sciences Based on analysis of the annual mean values of relative sunspot number during 1700 -- 2009, there are 3 components of solar cycles are confirmed: the first one is the usually well-known 11-yr cycle which has the strongest power; the second strongest solar cycle has the period of 103 years which can be named as Grand Cycle (marked as G1, G2, G3, and G4, respectively since 1700); the third component of solar cycle has a period of 51.5 years which is possibly the relatively weak second harmonic of the Grand Cycle. By using the similarity assumption, the author made an extrapolation of the forthcoming solar cycles after the cycle 23, and point out that solar cycle 24 will be in the vale between G3 and G4, it will be a relative long and weak solar active cycle, which may reach to its apex in about 2012-2014. As for the origin of solar cycles, the author believes the dynamo theory may be the best one to explain the 11-yr solar cycle, and speculates that the Grand Cycle is possibly resulted from the thermonuclear instability of the solar core which modulated the global energy releasing processes.
STP12 Abstracts Berlin, 12 - 16 July 2010 SCOSTEP Symposium 2010 Study of Quiet Solar Radio Emission at 1.0-7.6 GHz Band Tan Chengming Key Laboratory of Solar Activity, National Astronomical Observatories of Chinese Academy Sciences The quiet solar radio emission at 1.0-7.6 GHz band was studied with synthesis analysis of the observed data of Chinese solar broadband radio spectrometers and the numerical model of quiet solar radio emission. First, by analyzing the daily calibration data recorded by the solar radio spectrometers of China in the period of 1997-2007, some results were obtained. 1), the daily calibration coefficients were found in good correlation with local air temperature for most frequencies of 2.6-3.8 GHz band. 2) a set of constant calibration coefficient were fitted for three bands (1.0-2.0 GHz, 2.6-3.8 GHz, 5.2-7.6 GHz) of the spectrometers. 3) At 2.6-3.8 GHz band, a correction factor that varied with local air temperature was added to the constant coefficient calibration. For good channel (80 percent), the result shows the calibration error of correction coefficient and constant coefficient is 5-15 s.f.u and 5-20 s.f.u Then, with the analysis of calibration, the observed result of quiet solar radio emission flux at 1.0-7.6 GHz band was obtained. On the other hand, the numerical simulation of quiet solar radio emission is calculated in using of theory model. But the solar atmosphere parameter between the chromospheres and corona is still not quite certain. This work gave an appropriate result with the numerical simulation by adjusting the parameters properly.
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scostep 2010 (stp12) - Leibniz-Institut für Atmosphärenphysik an der ...

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